Annexe I : description des services d’observations labellisés liés à la planétologie

Consultation BDD

Service des éphémérides

Type

AA-ANO1

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

IMCCE Jacques LASKAR Jacques LASKAR [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA OCA Thierry LANZ Agnès FIENGA [email protected]

Description

L'IMCCE a la responsabilité, sous l'égide du Bureau des longitudes, de produire et de diffuser les calendriers et éphémérides au niveau national. Cette fonction est assurée l'institut par son Service des éphémérides. Aussi celui-ci a) produit les publications et éditions annuelles tout comme les éphémérides en ligne, b) diffuse les éphémérides de divers corps du système solaire - naturels et artificiels, et de phénomènes célestes, c) assure la maintenance et la mise jour des bases de données, d) procure une expertise juridique aux tribunaux, e) procure des éphémérides et données la demande pour les services similaires (USA, Japon), les agences, les chercheurs, les laboratoires et les observatoires. Consultation BDD

Gaia

Type

AA-ANO1, AA-ANO4

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OCA Thierry LANZ François MIGNARD [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA Frédéric ARENOU [email protected] IMCCE Jacques LASKAR Daniel HESTROFFER [email protected] OASU Marie Lise DUBERNET-TUCKEY Caroline SOUBIRAN [email protected] THETA Philippe ROUSSELOT Annie ROBIN [email protected] IAP Francis BERNARDEAU Brigitte ROCCA VOLMERANGE [email protected] ObAS Pierre-Alain DUC Jean-Louis HALBWACHS [email protected]

Description

Participation aux activités du Consortium DPAC (Data Processing and Analysis Consortium) pour la mission Gaia. Ceci comprend (i) la conception, la réalisation, la qualification et l'exécution des chaînes de traitement des données brutes du satellite devant aboutir la publication des produits Gaia, (ii) la validation des résultats et la production de l'ensemble de la documentation pour les utilisateurs chaque nouvelle remise de données (iii) la collecte d'informations complémentaires, nécessaires l'accomplissement de la mission, partir d'observations au sol. Consultation BDD

CHARA

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OCA Thierry LANZ Denis MOURARD [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUG Michel DIETRICH Karine PERRAUT [email protected] OSUL Isabelle DANIEL Isabelle TALLON-BOSC [email protected] Obs. Paris Claude CATALA Vincent COUDE DU FORESTO [email protected]

Description

Ce service a pour objectif le soutien aux groupes français exploitant l'interféromètre du Center for High Angular Resolution Astronomy (CHARA, USA). Ce réseau interférométrique optique situé l'observatoire du Mount Wilson (Californie) comprend 6 télescopes de 1 mètre sur des bases allant de 30 330 mètres, et est équipé de 2 instruments français: JOUFLU pour la recombinaison très haute précision dans l'infrarouge proche (bande K), et VEGA pour l'imagerie interférométrique dans le visible haute résolution spectrale et très haute résolution spatiale. D'autres instruments sont également en service: MIRC (pour l'imagerie interférométrique en bandes H et K, Université de Michigan), CLASSIC-CLIMB (pour une sensibilité maximale en bandes H et K, Chara Center), et PAVO un instrument 3T dans le visible pour la haute sensibilité (Université de Sydney). L’accès CHARA et donc l’hémisphère Nord ainsi qu’au domaine du visible est un atout très intéressant et complémentaire du VLTI.

Le soutien du service passe explicitement par les actions suivantes : 1) Soutien la préparation des observations et formation 2) Prise en charge des observations en mode service (dans le cadre de l’optimisation des nuits d’observation) et formation 3) Prise en charge/Soutien la réduction des données. Formation. 4) Maintenance technique, évolutions

Sur ce dernier point, l'équipe VEGA Nice a développé un prototype appelé FRIEND destiné comprendre le fonctionnement en interférométrie visible avec une correction partielle par optique adaptative sur chacun des télescopes de 1m. Ce prototype prépare le développement de l'instrument SPICA (recombinaison visible 6T fibrée). Consultation BDD

E-ELT / HARMONI

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUL Isabelle DANIEL Roland BACON [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU PYTHEAS Bruno HAMELIN Benoit NEICHEL [email protected] Description

Le spectrographe HARMONI est un des deux instruments de première lumière financés pour l’ELT européen.

Il s’agit d’un spectrographe intégral de champ (IFU) qui observera dans la gamme visible et proche infra-rouge (de 0.5 2.4 microns). HARMONI fournira une résolution spectrale de R=3000 R=20000, et une résolution angulaire de 60 4 mas. Pour exploiter pleinement la limite de diffraction de l’E-ELT, HARMONI sera équipé de deux systèmes d’Optique Adaptative (OA). Le premier est un système d’OA classique (SCAO) et le deuxième sera un système d’OA grand champ, assisté par étoiles lasers (LTAO). HARMONI s’inscrit dans la lignée d’instruments qui équipent le VLT, tels que SPHERE ou MUSE. La première lumière est prévue pour 2024. Les cas scientifiques principaux d’HARMONI couvrent un large spectre, depuis l’étude et la caractérisation des exo-planètes, l’étude des populations stellaire dans les galaxies proches, et jusqu’aux galaxies grand décalage vers le rouge.

HARMONI regroupe un consortium de 6 laboratoires, dont 2 laboratoires français : le LAM et le CRAL.

Le CRAL réalise les modules de découpage du champ et les optiques relai, le pipeline de réduction des données, et (avec l’IPAG), le contrôle de l’instrument. Un modèle numérique de l’instrument (INM) est en développement au CRAL pour simuler des données brutes HARMONI et tester les différentes étapes de réduction en lien avec les développements du pipeline.

Le LAM est en charge du développement des Optiques Adaptatives. Avec le LAM, l’IPAG est en charge du développement d’un bras d’imagerie haut-contraste permettant la caractérisation d’exoplanètes.

Les tâches de services proposées au CRAL sont les suivantes :

T1- Préparation de cas scientifiques clé pour tester le pipeline: Il s'agit d'extraire, partir de simulations astrophysiques ou d'observations existantes, des cas types d'observations simuler avec l'INM dans les principaux modes d'HARMONI (champs stellaires, galaxies, champs profonds), ainsi que des cibles spécifiques (cibles mouvantes, champs astrométriques). Ces données simulées serviront de test pour la réduction des données avec le pipeline. Ces résultats de réduction seront par ailleurs contrôlés dans une étape de validation par rapport aux données en entrée de l'INM, avec une quantification des erreurs et une étude de l'impact sur la science.

T2- Proposition et validation d’algorithmes avancés pour les particularités d’HARMONI: Il s'agit de contribuer la réflexion sur les choix d'algorithmes, puis leur validation, concernant les calibrations basées sur des observations du ciel: l'astrométrie, la correction des telluriques, et la soustraction optimale du ciel. En particulier, nous projetons d'utiliser le mode multi-lectures pour les détecteurs: il faudra exploiter cette possibilité de manière optimale pour les algorithmes ci-dessus.

T3- Participation au choix des tests de validation du pipeline qui seront effectuer en laboratoire et/ou sur le ciel au cours des phases de tests globaux puis de commissioning de l'instrument.

Les tâches de services proposées au LAM sont :

- Spécifications scientifiques de haut niveau et estimation de performances de l’instrument et des systèmes d’optique adaptative associés (SCAO et LTAO) sur la base des cas scientifiques prioritaires (formation et évolution des galaxies, formation stellaire, système solaire, exo-planètes, etc.) Ce travail inclut des activités de modélisation et/ou de simulation. Participation aux études systèmes, participation aux équipes scientifiques et techniques. - Spécification et préparation des logiciels d’acquisition et de réduction des données. Ce travail peut inclure des activités de démonstration et/ou de prototypage en laboratoire ou avec des démonstrateurs. Ces tâches devront évoluer au cours du cycle de développement de l’instrument vers des tâches de spécifications et d’étude de performance des sous-systèmes, puis de modélisation fine de ceux-ci, et enfin de caractérisation et de validation au cours des phases d’intégration et de tests puis de commissioning sur le ciel.

Les tâches de services proposées l’IPAG, sont : - Les spécifications scientifiques de haut niveau et l’estimation des performances du bras haut-contraste sur la base des cas scientifiques prioritaires (caractérisation d’exoplanètes, étude des disques de formation, etc.). Ce travail inclut des activités de modélisation et/ou de simulation ainsi qu’une participation aux études systèmes. - La préparation des outils de réduction des données : outils classiques d’imagerie différentielle & outils innovants exploitant la haute résolution spectrale de HARMONI pour détecter des signatures spectrales de diverses molécules. Ces tâches devront évoluer au cours du cycle de développement de l’instrument vers des tâches de spécifications et d’étude de performance du bras haut-contraste, puis de modélisation fine de celui-ci, et enfin de caractérisation et de validation au cours des phases d’intégration et de tests puis de commissioning sur le ciel. Consultation BDD

E-ELT / MICADO

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Yann CLENET [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUG Michel DIETRICH Gael CHAUVIN [email protected]

Description

MICADO, l’un des deux instruments de 1ère lumière de l’E-ELT, est une caméra spectro-imageur proche IR (bandes I, J, H et K) travaillant la limite de diffraction avec un champ de vue d’environ une minute d’angle. La résolution spectrale de son mode spectroscopique longue fente est environ de 8000. Développée sous le PI-ship du Max Planck Institut (MPE) de Garching, sa conception a été axée sur une très grande sensibilité et une très haute précision astrométrique. Avec son large champ, sa haute résolution angulaire, sa grande précision astrométrique et une sensibilité remarquable, MICADO aura ainsi les capacités de balayer une large gamme de sujets astrophysiques. Au sein du consortium, la France est responsable du mode d’optique adaptative de 1ère lumière de l’instrument, de type SCAO (proche de l’axe avec étoile naturelle), ainsi que des modes coronographique et masquage de pupille. Cette participation française est sous responsabilité LESIA, en partenariat avec le GEPI et l'IPAG. Le service d'observation correspond aux études, la réalisation, aux intégrations et tests et la recette sur le télescope de ces modes SCAO et haut contraste. Consultation BDD

SKA

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Willem VAN DRIEL [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUC Yves COQUET Gilles THEUREAU [email protected] OASU Marie Lise DUBERNET-TUCKEY Patrick CHARLOT [email protected] OCA Thierry LANZ Chiara FERRARI [email protected]

Description

L’objectif du projet international SKA (Square Kilometre Array) est la construction et l’exploitation scientifique d’un interféromètre radio géant opérationnel en ondes centimétriques métriques, d'une surface collectrice d'un kilomètre carré, dont la sensibilité sera 50 fois supérieure celle des plus grands instruments actuellement en opération ces fréquences. Consultation BDD

SPIRou

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Jean-Francois DONATI [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU PYTHEAS Bruno HAMELIN Isabelle BOISSE [email protected] OSUG Michel DIETRICH Xavier DELFOSSE [email protected] IAP Francis BERNARDEAU Guillaume HÉBRARD [email protected]

Description

SPIRou est la fois un spectropolarimètre et un velocimètre de haute précision fonctionnant dans le proche IR (0.98-2.35µm) donc les objectifs principaux sont (i) de détecter des exoterres habitables autour d’étoiles de faible masse, et (ii) d’étudier l’impact des champs magnétiques sur la formation des étoiles et des systèmes planétaires. SPIRou est un instrument de nouvelle génération pour le CFHT, dont l'installation sur site est prévue en 2017 et la mise en service pour la communauté en 2018. SPIRou doit notamment permettre d'accomplir un grand relevé de type Legacy de ~500 nuits, focalisé sur les deux objectifs scientifiques principaux du projet. Une copie de SPIRou pour le TBL (SPIP) est programmée pour 2020, sur un financement de la Région Midi-Pyrénées - Languedoc-Roussillon. Consultation BDD

VLTI / MATISSE

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OCA Thierry LANZ Bruno LOPEZ [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUG Michel DIETRICH Jean-Charles AUGEREAU [email protected]

Description

L'OCA, l'INSU et le laboratoire Lagrange, sont instituts et laboratoire 'Principal Investigateur' de l'instrument de seconde génération MATISSE au VLTI. Le service actuel assuré par les personnes en poste concerne la phase de commissioning sur le ciel de l'instrument ainsi que le développement et le maintien de l'Exposure Time Calculator de référence de MATISSE. La perspective d'optimisation de l'environnement VLTI en rapport avec MATISSE - par exemple le suiveur de frange externe GRA4MAT - amène de nouveaux besoins sur la période 2018-2020. Consultation BDD

Bepi Colombo / DBSC

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Fouad SAHRAOUI [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OVSQ Chantal CLAUD

Description

Le satellite Mercury Magnetospheric Orbiter (MMO) est l’une des deux sondes de la mission BepiColombo dont le but est l’exploration de la planète Mesure et de son environnement proche. La sonde MMO, sous la responsabilité de la JAXA, comporte une instrumentation complète dédiée aux mesures in-situ de l’environnement magnétisé de Mercure, incluant le vent solaire, la magnétogaine et la magnétosphère. L'instrument DBSC (Dual Band Search Coil) est un fluxmètre magnétique double bande parallèle l'axe de spin de la sonde MMO (Lead CoI Fouad Sahraoui, LPP, France). Il est l’un des instruments du consortium PWI (Plasma and Wave Instrument, PI : Yasumasa Kasaba, Univ. Tohuko, Japon). DBSC mesurera les fluctuations du champ magnétique dans deux bandes de fréquence : une bande BF couvrant la gamme [100mHz, 20kHz] et une bande HF [10,640] kHz. Deux fluxmètres magnétiques, construits par l'Université de Kanazawa (Japon), couvrent la même bande BF et forment un trièdre orthogonal avec le DBSC. Le LPP est responsable de la calibration des données de l’antenne HF et participera la calibration des données BF en collaboration avec l’équipe de l’université de Kanazawa. Les deux sondes MMO et MPO (Mercury Planetary Orbiter –sous la responsabilité de l’ESA) devraient être lancées en 2018 pour une insertion en orbite autour de Mercure en 2024. Consultation BDD

Bepi Colombo / MPPE

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Dominique DELCOURT [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OMP Michael TOPLIS Nicolas ANDRÉ [email protected]

Description

L'une des deux sondes de la mission Bepi Colombo vers Mercure (lancement prévu en octobre 2018 pour une insertion en orbite fin 2025) a pour objectif l'étude de l'environnement magnétisé de la planète et du vent solaire. Cette sonde MMO (Mercury Magnetospheric Orbiter) qui est sous la responsabilité de l'agence japonaise JAXA, comporte un ensemble d'instruments dédiés aux mesures des particules chargées et rassemblés dans le consortium MPPE (Mercury Plasma Particle Experiment, Principal Investigator : Yoshifumi Saito, ISAS, Japon). Parmi ces instruments, le spectromètre de masse ionique MSA (Mass Spectrum Analyzer, Principal Investigator : Dominique Delcourt, LPP, France) et les deux analyseurs d'électrons MEA (Mercury Electron Analyzer, Principal Investigator : Nicolas André, IRAP, France) sont sous responsabilité française. Tirant parti de la rotation de la sonde MMO (période de spin de 4 s), l'instrument MSA mesurera les fonctions de distribution tri-dimensionnelles d'ions magnétosphériques sur une large gamme de masses (1-60 uma) et d'énergies (1 eV/q - 38 keV/q). MSA consiste en un analyseur sphérique de type "top-hat" pour la sélection en énergie, suivi d'une chambre temps de vol pour l'identification des masses. Utilisant le principe "réflectron", cette chambre temps de vol est polarisée avec un champ électrique linéaire qui permet d'obtenir une haute résolution en masse (typiquement, m/Dm > 50), ce qui permettra notamment de distinguer les ions 39K des ions 40Ca. L'instrument MSA permettra ainsi d'identifier les différentes espèces en présence dans le milieu, d'étudier leur dynamique et ce faisant de caractériser l'interaction du vent solaire avec la planète. De leur côté, les deux analyseurs "top-hat" MEA fourniront pour la première fois des mesures des fonctions de distribution tri-dimensionnelles d'électrons dans la magnétosphère de Mercure. Ces mesures dans une large gamme de flux et d'énergies (1 eV/q - 30 keV/q) permettront d'étudier la dynamique de la magnétosphère et d'en caractériser les courants. Consultation BDD

Bepi Colombo / PHEBUS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OVSQ Chantal CLAUD Eric QUEMERAIS [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

PHEBUS (pour Probing of Hermean Exosphere By Ultraviolet Spectroscopy) est un double spectromètre couvrant les gammes de l'extrême ultraviolet (EUV: 55-155 nm) et du lointain ultraviolet (FUV: 145-315 nm) dédié la caractérisation de l'exosphère de Mercure en termes de composition et de dynamique, et des relations entre la surface et l'exosphère. Cet instrument, sous responsabilité française, est réalisé en coopération avec le Japon (détecteurs), la Russie (système de pointage) et l'Italie (étalonnage au sol). Les principaux objectifs scientifiques de PHEBUS sont les suivants : détermination de la composition et de la structure verticale de l'exosphère; caractérisation de la dynamique exosphérique: circulation jour-nuit, transport des régions actives aux régions inactives; étude des processus de surface l'origine de l'exosphère; identification et caractérisation des sources de constituants exosphériques; détection et caractérisation de l'ionosphère et de sa relation avec l'exosphère neutre; suivi spatial et temporel des échanges exosphère/magnétosphère et des processus de transport; étude et quantification de l'échappement, de l'équilibre sources/puits l'échelle globale et des cycles géochimiques en synergie avec d'autres expériences de BepiColombo (MSASI, MPPE sur MMO; MIXS, SERENA sur MPO). Consultation BDD

Bepi Colombo / PICAM

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OVSQ Chantal CLAUD François LEBLANC [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA

Description

L'instrument PICAM/Bepi-Colombo (PI: H. Lichtenegger, IWF, Autriche) fait partie d’un consortium particule SERENA (PI : S. Orsini, INAF, Italie) a pour objectif de mesurer l’environnement ionisé de la planète Mercure. Il a été conçu et en partie réalisé par le LATMOS et le LPP. Le LATMOS et LPP ont notamment la responsabilité du détecteur, d'une partie de l'optique électrostatique et de la modélisation numérique de l'instrument. Ces outils numériques développés par le LATMOS seront indispensables pour l'exploitation future des mesures réalisées par cet instrument. Ils sont l'objet d'un travail continu de mise jour notamment par comparaison avec les dernières calibrations de l'instrument. Ils seront indispensables pour calibrer les données de cet instrument. Consultation BDD

Bepi Colombo / SimbioSys

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUPS Nabila AGHANIM Yves LANGEVIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA Alain DORESSOUNDIRAM [email protected]

Description

Le service concerne la fourniture et le suivi des contributions françaises au consortium instrumental "Simbio-Sys" (HRIC : caméra HR, STC : caméra stéréo, VIHI : spectromètre imageur VIS-NIR) en collaboration avec l'Italie ("lead funding agency") et la France sur la mision BepiColombo de l'ESA dédiée l'étude de Mercure - module électronique mutualisé (OSUPS / IAS) - étalonnage intégré du complexe Simbio-sys (OSUPS / IAS) - électronique de proximité VIHI (Observatoire de Paris / LESIA) - fourniture et caractérisation du détecteur VIHI (Observatoire de Paris / LESIA) Consultation BDD

Bepi Colombo / SORBET-PWI

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Michel MONCUQUET [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Description

Sorbet est un récepteur radio HF, conçu et réalisé au LESIA, et couvrant la gamme . Cet instrument est embarqué sur le satellite japonais MMO (JAXA), qui forme avec le satellite MPO (ESA) la mission BepiColombo, qui sera lancée en octobre 2018 (ou backup en Avril 2019) et arrivera Mercure en 2025-2026. Sorbet constitue donc la composante radio-HF du consortium d'instruments PWI (Plasma Waves Investigation, PI: Yasumasa Kasaba, Université de Tohoku, co-PI: Michel Moncuquet, observatoire de Paris-LESIA), et mesure des spectres de champs électriques et magnétiques dans la gamme 2.5kHz-10MHz. Il est raccordé deux antennes électriques et un search coil magnétique(réalisé au LPP). Michel Moncuquet est aussi responsable (lead co-I), au sein du consortium PWI, de l’instrument Sorbet, et il a donc la responsabilité des tests d'intégration sur le satellite, des étalonnages et calibrations avant le lancement, puis de la chaîne de traitement des télémesures et des calibrations en vol (qui sera effectuée au LESIA-Observatoire de Paris sur un serveur dédié), et enfin la mise disposition des données en valeurs physiques (sur serveur de l'OP également) puis des données plus forte valeur ajoutée scientifique (par exemple, densités et températures électroniques par spectro QTN). Ces données seront mises disposition de l'équipe PWI uniquement dans un premier temps (< 3mois) puis toute la communauté scientifique (via la JAXA, et très probablement au CDPP). L'ensemble de ces responsabilités définit ce service d'observation, qui correspond 1/3 ETP ( comprendre en plus des personnels hors CNAP qui participent au service), depuis la phase d'étalonnage (2012_2016) et pendant la phase de préparation des traitements et opérations jusqu’au lancement et recette en vol (2017-2019). La phase de croisière (2019-2025) est explicitée plus en détail ci dessous et devrait nécessiter davantage d’ETP, comme sans doute la phase d'exploitation des données radio HF produites partir de 2025 qui devra être définie dans le cadre d’une ANO5, mais une évaluation en ETP plus précise est difficile anticiper.

En ce qui concerne la phase actuelle (qui suit la phase d’étalonnage, désormais achevée, de l'instrument SORBET) il s’agit de préparer/simuler l’instruments et de définir les modes opératoires jusqu’a la recette après lancement (2017-2019). Il s’agit aussi de se donner une pratique préalable (avant lancement) de la chaîne de traitement sur des données simulées (et d’initier ainsi la phase “de croisière” 2019-2025 -voir ci-dessous). Cette tâche est actuellement assurée principalement par Michel Moncuquet, IRHC , co-PI PWI, par Filippo Pantellini, Astronome, co-I PWI, et par Léa Griton, Doctorante, Associate Scientist PWI, tous les trois au pôle plasma du LESIA.

En ce qui concerne la description d’une phase intermédiaire (2019-2025) d’un service national d'observation radio HF/BepiColombo, ANO2, commençons par une remarque importante: il n'y a pas de phase de croisière proprement parler concernant SORBET, le satellite MMO étant recouvert d'une coiffe qui n'est larguée qu'l'arrivée Mercure, puis séparation des deux satellites MMO et MPO, puis déploiement des antennes. SORBET sera donc en mode veille pendant les 7 années de croisière, avec des phases de recettes et de calibrations internes, mais aucunes mesures scientifiquement exploitables. C'est pourquoi nous voudrions mettre en oeuvre la chaîne de traitement en utilisant des simulations d'environnement électromagnétiques de Mercure (développé au labo sous la responsabilité de F. Pantellini, qui a beaucoup participé la définition/conception de l'instrument) et créer ainsi un signal artificiel (en simulant aussi SORBET), que nous injecterons dans la chaîne de traitement complète. L'objectif est triple: 1) tester la réactivité de notre chaîne de traitement aux phénomènes attendus ou simplement suspectés (notamment les logiciels de détection automatique d'évènement). 2)le débit de télémesure est extrèmement contingenté sur MMO-BepiColombo, et la plupart des mesures ne serons pas transmises au sol: il faudra sélectionner drastiquement bord, sur les bons critères, et prévoir les modes de mesures télécommandés dans un temps assez bref au vu des premiers résultats. Une pratique préalable de la chaîne de traitement sur des données "plausibles" serait un atout. 3) anticiper les mesures et les confronter ce que nous voyons réellement est un excellent moyen d'être surpris, et de comprendre nos erreurs, donc de faire de la bonne science (mais on sort du cadre d'un service d'observation). En résumé, cette définition d’un SNO SORBET/BepiColombo de 2019 2025, incluant une forte partie “simulation numérique” et dont Filippo Pantellini serait leader, est en cours de conception. Consultation BDD

Cassini-Huygens / RPWS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Baptiste CECCONI [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

La mission Cassini-Huygens est arrivée Saturne en juillet 2004 et observe la planète et son environnement en continu depuis lors. L'instrument RPWS (Radio and Plasma Waves Science) est dédié l'exploration de la magnétosphère de Saturne.

Le LESIA a conçu et réalisé le récepteur HFR (High Frequency Receiver) qui couvre la gamme 4 kHz - 16 MHz. Le LPP a conçu et réalisé l'antenne magnétique tri-axiale (Search-Coil magnetometer) qui analyse la composante magnétique des ondes dans la gamme 1 Hz-12 kHz travers les analyseurs de spectres LFR,MFR, et les analyseurs de forme d'onde (WFR, WBR).

Le service rassemble les activités d’étalonnage, d’exploitation et de distribution des données liées aux instruments dont le LESIA et le LPP ont la responsabilité. Ces activités sont : - Définition des modes d'observation. - Étalonnages. - Récupération des données N0 auprès de l'institut P.I. (Université d'Iowa, USA). - Fabrication des données N1, N2, N3, mise disposition de la communauté. - Elaboration d'outil de visualisation des données sommaire destiné l'exploration rapide et visuelle du jeu de données produit. - Production de jeux de données valeur ajoutée (Goniopolarimétrie, Bruit Thermique, Sondeur). - Construction des jeux de données archiver auprès des centres de données NASA/PDS et CNES/CDPP. Consultation BDD

Cassini-Huygens / VIMS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUNA Thierry LE BEAU Christophe SOTIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Préparation de séquences d’observation de titan par le spectro-imageur VIMS Visible Infrared Mapping Spectrometer bord de la sonde spatiale Cassini. Consultation BDD

ExoMars / CLUPI

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUC Yves COQUET Frances WESTALL [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Le projet CLUPI se place dans le contexte de la mission ESA ExoMars 2018, de son rover martien, et de sa charge utile scientifique Pasteur.

L’instrument CLUPI est une caméra d’imagerie rapprochée couleur qui est l’équivalent de la loupe du géologue de terrain.

Pour les chercheurs orléanais impliqués, le projet CLUPI est une composante de leur projet Mars-GeoMicroPal actuel dont il partage les objectifs scientifiques: recherche de traces de vie actuelle ou fossile sur Mars, caractérisation de ses habitats potentiels dans les roches et sols examinés.

La démarche scientifique consiste utiliser les instruments d’observation optique disponibles bord du rover, tous les grossissements, ainsi que les instruments géochimiques, pour la recherche de traces de vie actuelle et fossile dans un cadre géologique, paléo-environnemental et micropaléontologique. Cette recherche commencera par la caractérisation du contexte géologique sur une gamme d’échelles qui va du panoramique jusqu’au microscopique. L’observation des échantillons de roche ou de régolite, de l’échelle de 100 microns environ l’échelle de quelques 10 microns avec CLUPI, en combinaison avec les données fournies par les spectromètres infrarouge et le spectromètre Raman contribuera comprendre la nature du matériau, sa composition, son mode de formation, ainsi que les processus qui ont altéré la roche ou le régolite depuis sa formation. La compréhension du contexte géologique est fondamentale pour l’interprétation de la biogénicité d’éventuelles biosignatures et l’instrument CLUPI un maillon indispensable dans l’analyse d’un échantillon entre les instruments extérieurs du rover et le laboratoire d’analyse, dépourvu de microscope optique visible, l’intérieur du rover. Consultation BDD

ExoMars / MicrOmega

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUPS Nabila AGHANIM Jean-Pierre BIBRING [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA

Description

Le service d’observation MicrOmega / ExoMars porte sur l‘ensemble des activités liées au développement, tests, qualification et étalonnage de l’Instrument MicrOmega, sélectionné pour être intégré au laboratoire d’analyse in situ des échantillons martiens bord du rover de la mission ExoMars 2020 de l’ESA. MicrOmega consiste en un microscope imageur hyperspectral, travaillant dans le domaine 0,5 – 3,6 µm, avec plus de 320 canaux spectraux : de chaque échantillon, MicrOmega acquerra un cube-image tridimensionnel (x,y,?), dans lequel chaque pixel des images, de 20 µm de large (le champ de vue de 5 mm est imagé par 256 x 256 px2) sera caractérisé par son spectre dans le visible et le proche infrarouge. Dans ce domaine spectral, la plupart des constituants potentiels, minéraux ignés et altérés, glaces et organiques, ont des signatures diagnostiques : MicrOmega permettra donc de mettre en évidence, pour la première fois l’échelle microscopique, la composition des grains martiens, et d’identifier et de localiser des phases d’intérêt exobiologiques : minéraux aqueux (phyllosilicates, sulfates ou carbonates), et des composés carbonés (aliphatiques ou aromatiques) qui leur seraient couplés. Parce qu’elles sont non destructives, ces observations permettront ensuite de localiser, sous deux autres instruments (RLS et MOMA), les grains d’intérêt, pour en compléter l’analyse. MicrOmega est développé sous la responsabilité scientifique et technique de l’IAS (personnels CNRS, Université et Observatoire), grâce un soutien financier spécifique du CNES. Les opérations au sol auront lieu partir de mi-2021. Elles exigeront que le traitement des mesures d’étalonnage soit achevé sous la forme d’exécutables, afin de permettre le traitement en temps réel des données qui seront transmises dès leur acquisition, critiques pour les décisions opérationnelles qui devront être prises quant au planning journalier du rover. Consultation BDD

ExoMars / MOMA-GC

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

EFLUVE Matthias BEEKMANN François RAULIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OVSQ Chantal CLAUD Cyril SZOPA [email protected]

Description

MOMA-GC est un chromatographe en phase gazeuse (GC), constituant un sous ensemble de l’instrument MOMA (Mars Organic Matter Analyser) dont le PI est Fred Goesmann (Max Planck, Lindau, Allemagne). MOMA est l’un des instruments de la charge utile du rover de la mission ExoMars (ESA-Roscosmos) 2020. MOMA est un ensemble d’instrumentation GC-MS et LD-MS (GC couplée la spectrométrie de masse et désorption laser (LD) couplée la spectrométrie de masse. Il permettra l’analyse moléculaire du sol de Mars, en particulier l’analyse des composés organiques, volatils et réfractaires, ainsi que l’analyse isotopique et chirale. MOMA-GC comprend 4 colonnes chromatographiques, dont une colonne chirale, et utilise la dérivatisation chimique pour l’analyse des composés peu ou pas volatils.

Références :

W. Goetz, W. B. Brinckerhoff, R. Arevalo, C. Freissinet, S. Getty, D. P. Glavin, S. Siljeström, A. Buch, F. Stalport, A. Grubisic, X. Li, V. Pinnick, R. Danell, F. H. W. van Amerom F. Goesmann, H. Steininger, N. Grand, F. Raulin, C. Szopa, U. Meierhenrich, J. R. Brucato and the MOMA Science Team (2016). MOMA: the challenge to search for organics and biosignatures on Mars. Int. J. Astrobio. 15 (3), 239-50.

F. Goesmann, W. B. Brinckerhoff, F. Raulin, W. Goetz*, R. Danell4 S. Getty, S. Siljeström, H. Steininger, R. Arevalo Jr., A. Buch, C. Freissinet, A. Grubisi2, U. Meierhenrich, H. Mißbach, V. Pinnick, F. Stalport, C. Szopa, J. R. Brucato, D. P. Glavin, N. Grand, X. Li, F. H. W. van Amerom, and the MOMA Science Team (2017). The Mars Organic Molecule Analyzer (MOMA) Instrument: Characterization of Organic Material in Martian Sediments Astrobiology, 17 (6-7), 655-685. DOI: 10.1089/ast.2016.1551. Consultation BDD

ExoMars / RLS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Sylvestre MAURICE [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

ExoMars est la première mission mobile de l’ESA la surface de Mars. Son objectif est de chercher des traces de vie la surface de la planète rouge. RLS (Raman Light Spectrometer) est un des instruments du laboratoire embarqué sur la sonde qui étudiera par spectroscopie Raman les échantillons du sol de Mars prélevés 2 m de profondeur. La sonde ExoMars sera lancée en juillet-août 2020 et se posera sur Mars 8 mois plus tard. Le projet ExoMars a démarré en 2004. Il a subi plusieurs revers programmatiques mais est maintenant consolidé pour ce décollage en 2020. La France en la personne de S. Maurice est co-PI de l’instrument RLS en partenariat avec F. Rull (Université de Valladolid). Nous sommes responsables de la fourniture du boitier électronique de toute l’expérience, l’Espagne fournissant les parties optiques (spectromètre et tête optique). La calibration de l’instrument est faite en Espagne et l’analyse des données en France.

Le SNO ne concerne que la partie française de ExoMars, savoir le boitier ICEU. Le SNO a pour objectif de soutenir scientifiquement et techniquement la construction de l’instrument ExoMars/RLS, la construction des outils d’analyse et de gestion des données. Consultation BDD

ExoMars / WISDOM

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OVSQ Chantal CLAUD Valérie CIARLETTI [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OASU Marie Lise DUBERNET-TUCKEY OSUPS Nabila AGHANIM

Description

Il s’agit d’acquérir des données caractérisant les structures du sous-sol martien et de mettre ses données la disposition de la communauté de planétologie. L’instrument en question WISDOM (Water Ice Subsurface Deposits Observation on Mars) est en cours de développement pour la mission ExoMars 2020. Il est conçu et développé au LATMOS avec l'aide de l’OAB de Bordeaux. Aucune donnée n’est actuellement disponible. Consultation BDD

InSight / SEIS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

IPGP Marc CHAUSSIDON Philippe LOGNONNÉ [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUNA Thierry LE BEAU Antoine MOCQUET [email protected] OCA Thierry LANZ Lucie ROLLAND [email protected]

Description

L’objectif principal du service sera d’accompagner la mission INSIGHT, qui déploiera en novembre 2018 un Observatoire Géophysique la surface de la planète Mars, réalisant des mesures sismiques, géodésiques et magnétiques simultanées. Cet observatoire Martien est dans la logique des SNO de la section AA associés aux autres missions d’Exploration du Système solaire, avec tout la fois des phases de développement, opérations, et d’archivage. Si la durée de vie nominale d’InSight est d’une année Martienne (deux années terrestres), il est fortement probable que la mission pourra continuer ses opérations pendant plusieurs années, l’instar des MER dont l’un d’eux est aujourd’hui en opération depuis plus de 10 ans. L’IPGP est responsable de l’instrument principal de la mission (expérience SEIS), de la livraison des capteurs très large bande passante (VBB) de ce dernier, et de deux services: le Mars Data Service, chargé de la diffusion et de l’archivage des données SEIS, et le Mars Structure Service, chargé de l’analyse de ces données et de la détermination des modèles de structure interne de Mars, en co-responsabilité avec les géophysiciens du Laboratoire de Planétologie et Géodynamique de Nantes (LPG, UMR 6112) au sein de l'OSUNA (UMS 3281). Il est cependant noter que les données d’INSIGHT seront diffusées la communauté internationale suivant des règles proches de celles des observatoires sismologiques, avec un temps de latence de 90 jours jusqu’mi 2019, réduit par la suite moins de 30 jours dès Juin 2019, et qu’une distribution de ces données des fins pédagogiques est prévue avec GéoAzur, au sein de l’OCA, dans le cadre du réseau Sismo l’Ecole. L’ISAE, établissement hors-INSU, qui est, avec l’ETH de Zürich, impliqué dans le Mars Quake Service, chargé de la détection et de la localisation des séismes, soutiendra les activités d’opération. D’autres projets sont enfin l’étude pour poursuivre l’approche scientifique d’InSight, que cela soit sur la Lune (MoonRise/NASA, Lunar Geophysical Network/NASA, ChangE/CSA) ou sur Mars (Nspire/ESA). Ils pourraient voir le jour pour des lancements dès 2022. Une autre vocation de ce service sera donc de poursuivre le développement et la fourniture d’instruments géophysiques pour ces futurs réseaux planétaires, avec des activités de R&T développées dans le cadre du Labex UnivEarth entres les laboratoires spatiaux de l’IPGP et d’APC par exemple. Dans le cas de la sismologie planétaire, ce besoin est de plus renforcé par une forte exigence en terme de sensibilité et de bruit sur les instruments: tant la Lune que Mars ont des activités sismiques bien plus faibles que la Terre, ce qui implique le développement et la qualification scientifique d’instruments de très bas bruit, relativement complexes du point de vue technologique, en particulier avec les contraintes de masse, de puissance, d’environnement, de chocs et de vibrations propres aux missions spatiales. Consultation BDD

JUICE / MAJIS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUPS Nabila AGHANIM Yves LANGEVIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA

Description

Ce service SO2 est dédié la réalisation puis aux opérations en vol du spectromètre imageur MAJIS sur la mission JUICE, 1ère mission majeure ("L" pour large) du programme Cosmic Vision de l'ESA. Cette mission est dédiée au système de Jupiter, avec des survols rapprochés de Europe, Callisto et Ganymède et des observations de Jupiter suivies d'une mise en orbite circulaire polaire autour de Ganymède, le plus gros satellite du système solaire (5260 km de diamètre).

L'IAS (OSUPS) assure la responsabilité scientifique et technique de l'instrument ainsi que la réalisation du module électronique central, des électroniques de proximité et des plans focaux. le LESIA (Observatoire de Paris) est responsable de la production des cubes "géométriques" (position, distance, incidence, émergence et phase pour chaque pixel) dans le contexte du segment sol. Consultation BDD

JUICE / PEP

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Nicolas ANDRE [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

La mission JUICE (Jupiter ICy moon Explorer) a été sélectionnée début 2012 parmi 3 missions candidates pour être la première «grande » mission (L1) du plan « Cosmic Vision » 2015-2025, nouveau cycle de programmation du programme scientifique obligatoire de l’Agence Spatiale Européenne. La mission JUICE sera lancée en 2022 et a pour objectifs l’étude de l’habitabilité et du fonctionnement du système jovien (Jupiter, la magnétosphère et ses satellites Europa, Ganymède, et Callisto). La mission JUICE a été adoptée par le SPC de l’ESA fin 2014. Parmi les 11 instruments de JUICE, PEP (Particle Environment Package) est une suite instrumentale de 6 senseurs destinés caractériser l’environnement de particules de différentes énergies et polarisations de l’environnement de la planète Jupiter et de ses satellites. La contribution instrumentale de l’IRAP au consortium PEP sous responsabilité de l’IRF Kiruna (Suède) et de l’Université de Berne (suisse) consiste en, d’une part, la fourniture et la caractérisation des détecteurs MCP (MicroChannel Plates) de l’instrument JENI (Jupiter Energetic Neutrals and Ions), et, d’autre part, la réalisation des tests de caractérisation des performances sous radiations des divers détecteurs de particules qu’embarque la suite instrumentale PEP. JENI est un détecteur de particules ionisées opérant dans la gamme d’énergie 500 eV - 300 keV pour les ENA, et 500 eV - 5 MeV pour les ions, développé sous la responsabilité du JHU/APL (USA). Consultation BDD

JUICE / RPWI

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Baptiste CECCONI [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUC Yves COQUET Pierre HENRI [email protected] OVSQ Chantal CLAUD Ronan MODOLO [email protected] OMP Michael TOPLIS Vincent GENOT [email protected] Description

La mission JUICE (Jupiter Icy Moon Explorer) a été adoptée l'automne 2014 et ses instruments scientifiques sont en phases de développement. L'instrument RPWI (Radio and Plasma Waves Instrument) est constitué de plusieurs récepteurs reliés des senseurs électriques et magnétiques couvrant la partie basse fréquence du spectre (quelques Hz 45 MHz). Les objectifs scientifiques principaux sont, d'une part, l'exploration de la magnétosphère de Jupiter, du rôle des satellites galiléens sur son activité et son interaction avec le vent solaire; et d'autre part, l'exploration de Ganymède, l'étude de son champ magnétique interne et de son interaction avec la magnétosphère de Jupiter. Les laboratoires français impliqués dans l'instrument RPWI sont le LESIA, le LPP, le LPC2E, le LATMOS et l'IRAP. La participation française l'équipe RPWI est coordonnée par son co-PI français, B. Cecconi, au LESIA. Les responsabilités des différents laboratoires en termes de SNO sont les suivantes : - Le LESIA est aussi responsable de la coordination scientifique de JENRAGE (Jovian Environment Radio Astronomy and Ganyede Exploration), l'instrument radio basse fréquence, conçu en collaboration avec la Suède et le Japon. Le LESIA fournit le savoir faire et l'expérience acquise sur les projets précédents (en particulier Cassini/RPWS et STEREO/Waves), en ce qui concerne la conception de l'instrument. Il prépare son étalonnage au sol et en vol, ainsi que les modes opératoires instrumentaux, et met en place de chaîne de traitement pour l'analyse des données, et prépare l'archivage et de la distribution des données obtenues par cet instrument. - Le LPP conçoit et construit un Search Coil 3D, capteur magnétique de RPWI (héritage Cassini/RPWS, BepiColombo/MMO/RPW, notamment), prépare son étalonnage au sol et en vol, met en place la chaine de traitement des données en collaboration avec l'équipe Tchèque qui construit le récepteur associé, et prépare l'archivage et la distribution des données issues de ce capteur. - Le LPC2E conçoit et construit l'expérience MIME (Mutual Impedance Measurements) avec l'héritage de l'expérience MIP de la mission Rosetta. L'équipe prépare les modes opératoires instrumentaux, l'étalonnage de l'instrument, effectue les modélisations numériques nécessaires l'interprétation des mesures. Il prépare aussi l'archivage et de la distribution des données obtenues par cet instrument. - Le LATMOS fournit un support toute l'équipe RPWI pour la modélisation de l'environnement spatial autour de Jupiter et de Ganymède. - L'IRAP, en particulier travers le CDPP, fournit un soutien pour la mise en place de l'archivage et de la distribution des données issues de l'expérience RPWI toute entière. Il fournit aussi des outils permettant de préparer les observations de RPWI en utilisant les modèles fournis par le LATMOS. Consultation BDD

JUICE / SWI

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Emmanuel LELLOUCH [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OASU Marie Lise DUBERNET-TUCKEY Françoise BILLEBAUD [email protected]

Description

- Fourniture de sous-systèmes pour l’instrument SWI (Submillimeter Wave Instrument) sur la mission JUICE (mission L1 de l’ESA)

- Préparation des étapes (caractérisation et calibration de l’instrument, définition des stratégies d’observations, uplink/downlink/archivage) nécessaires l’acquisition, l’analyse, et la mise disposition de la communauté des observations Consultation BDD

JUICE / UVS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OVSQ Chantal CLAUD Eric QUEMERAIS [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

La mission JUICE de l'agence spatiale européenne est dédiée l'étude du système de Jupiter et des ses lunes, principalement Callisto, Ganymède et Europe. Elle sera lancée en 2022 pour une arrivée dans le système de Jupiter en 2030. L'instrument UVS est un spectromètre ultraviolet (55nm-210nm) qui permettra de caractériser les émissions des atmosphères et surfaces des lunes de Jupiter, de la haute atmosphère de Jupiter aisi que du tore d'Io. Cet instrument est fourni par le Southwest Research Institute (PI R. Gladstone, San Antonio, Texas). Le LATMOS coopère a la réalisation de l'instrument par la caractérisation et la fourniture des réseaux de diffraction. Consultation BDD

JWST / MIRI

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Externe OSU : AIM Anne DECOURCHELLE Pierre-Olivier LAGAGE [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUPS Nabila AGHANIM Alain ABERGEL [email protected] Obs. Paris Claude CATALA Anthony BOCCALETTI [email protected] PYTHEAS Bruno HAMELIN Olivier LE FEVRE [email protected]

Description

- Développement des instruments et logiciels du télescope spatial JWST et plus particulièrement de l'imageur de l'instrument infrarouge moyen MIRI (5-28 microns) et de ses 4 modes d'observation : imagerie,coronographie (notamment par masques de phase 4 quadrants), spectroscopie par fente basse résolution (R=100) spectroscopie, spectroscopie sans fente (pour l'observations du transit/eclipse d'exoplanètes). - Participation au centre d'expertise français - Préparation des campagnes d'observation avec le JWST Consultation BDD

Mars Express / OMEGA

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUPS Nabila AGHANIM Jean-Pierre BIBRING [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA

Description

Le service d'observation "Mars Express / OMEGA" (ASO SO2) porte sur toutes les activités liées la réalisation du modèle de vol de l'instrument OMEGA embarqué sur la mission Mars Express de l'Agence Spatiale Européenne. OMEGA (Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité) est un imageur spectral dans le visible et le proche infrarouge qui a obtenu des résultats majeurs sur l'histoire et l'évolution de surface de Mars. Le service d'observation SO2 OMEGA/Mars Express a tout d'abord porté sur les activités de réalisation d'OMEGA, sur la base du modèle de rechange de l'instrument embarqué sur la sonde russe Mars 96 (échec au lancement) pour la caméra et d'un module électronique développé en parallèle avec les instruments sous responsabilité IAS de la mission Rosetta. Le SO2 OMEGA/Mars Express a ensuite porté sur l'étalonnage au sol (2002). Depuis la mise en orbite (24 décembre 2003), l'activité principale dans le contexte de ce service SO2 est la préparation des opérations scientifiques depuis la mise en orbite autour de Mars le 24 décembre 2003 et la validation de données de niveau 2 (décommutées et décalibrées) pour mise disposition des co-investigateurs puis archivage. Ces activités se poursuivent actuellement, avec une mission qui a été étendue jusqu'fin 2018. Une demande de prolongation de deux ans est en cours d'évaluation par l'Agence Spatiale Européenne. Elles s'appuient sur un soutien budgétaire du CNES (y compris des supports CDD) et des ressources humaines IAS (personnels CNRS, chercheurs / IT et personnels statut universitaire, EC / CNAP). Depuis début 2016, les données produites par le service SOS Mars Express / OMEGA sont intégrées dans les cartes et autres produits de niveau 3 et plus dans le contexte du SO5 PSUP. Consultation BDD

Mars Express / SPICAM

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OVSQ Chantal CLAUD Franck MONTMESSIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

La mission de l'ESA Mars Express est en opérations autour de Mars depuis 2004. Dans ce cadre, le LATMOS est responsable de l'instrument SPICAM, un spectromètre couvrant les gammes ultraviolet et infrarouge pour la caractérisation de l'atmosphère martienne. Le développement de l'instrument et son exploitation ont été et restent soutenus par le CNES.

SPICAM est chargé de réaliser un relevé précis de la composition de l’atmosphère de Mars et aussi dans une moindre mesure de sa surface en sondant dans les gammes UV et IR.

Les données de l’instrument sont réceptionnées, traitées, exploitées et analysées par notre équipe d’ingénieurs et de scientifiques au LATMOS. Une grande partie de l'effort concerne la mise sous archive des données dans un format décidé par l'ESA (reprenant celui du Planetary Data System de la NASA).

A noter qu'une dégradation très nette du canal UV compromet le recueil d'observations depuis aout 2011. Cependant, une base de données de plus de 10 ans a pu être constituées, permettant d'étudier l'atmosphère de Mars et son climat sur des échelles diurnes, saisonnières et pluri-annuelles.

Depuis l'année 2014, l'équipe réalisé l'archivage des données dites de niveau 1A où sont assemblées des données nettoyées du courant d'obscurité, des effets dits de "cosmiques" ainsi que des changements intempestifs du gain de la chaine de détection.

A la fin de l'année 2014, la canal UV a cessé de retransmettre des données scientifiques, l'intégralité de l'analyse s'est donc reportée sur le canal proche-infrarouge. Consultation BDD

Mars Science Laboratory / ChemCam

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Sylvestre MAURICE [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUG Michel DIETRICH Eric LEWIN [email protected] OSUNA Thierry LE BEAU Nicolas MANGOLD [email protected] OSUPS Nabila AGHANIM Yves LANGEVIN [email protected]

Description

La mission Mars Science Laboratory (MSL) de la NASA et du JPL a déposé le rover Curiosity la surface de Mars en août 2012. Le rover a 4 objectifs majeurs : l’habitabilité passé du site, la géologie et la géochimie aqueuse des sédiments anciens, son évolution climatique et géologique et le niveau de radiation pour les prochaines missions habitées.

Dans ce contexte ChemCam fournit une analyse de la chimie distance sans que le rover n’ait a changé de position grâce la technique LIBS : il s’agit d’un laser ablation qui transforme la roche en plasma et analyse l’émission de photons crées lors du refroidissement de ce plasma par des spectromètres. Les principaux éléments chimiques utiles la compréhension de la géologie sont identifiables l’échelle millimétrique, y compris les volatils (H, C, O, S, F, Cl) intérêt exobiologique. ChemCam est aussi doté d’un imageur haute résolution qui permet d’observer les cibles analysées. Curiosity se déplace et/ou procède des analyses tous les jours depuis plus de trois ans. Il a effectué 12 km la surface de Mars. Le long de sa route, ChemCam a mesuré la composition de plus de 1 000 cibles avec plusieurs centaines de tirs laser sur chacune (et plus de 300 000 tirs laser ce jour au total). L’instrument est utilisé en moyenne une deux heures, un jour sur deux. ChemCam a ainsi joué un rôle clé dans les analyses géochimiques du rover Curiosity dans le cratère Gale depuis les premières analyses. L’ensemble des données est mis la disposition de la communauté sur le Planetary Data System.

Le SNO se charge d’animer la communauté autour des données de ChemCam, de mettre disposition les données sur le PDS, de participer aux opérations quotidiennes, de valoriser les données de l’instrument. Nous décrivons cela en section B sous forme de Work Package (WP). Les WP 2 4 (opérations, calibration, réduction de données) constituent le socle du SO ChemCam.

Cet instrument se trouve l’intersection des préoccupations du CNAP AA, de la section 17 et la section 18 du CNRS. Consultation BDD

Mars Science Laboratory / SAM-GC

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

EFLUVE Matthias BEEKMANN Patrice COLL [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OVSQ Chantal CLAUD Cyril SZOPA [email protected]

Description

SAM-GC est un chromatographe en phase gazeuse (GC) miniature, et est un des 3 instruments de la suite instrumentale SAM (pour Sample Analysis at Mars), PI Paul Mahaffy (NASA Goddard Flight Center, Maryland, USA). Cette suite instrumentale est l’élément central de la charge utile du rover Curiosity de la mission Mars Science Laboratory (MSL/NASA). Cette suite comprend également un spectromètre de masse quadripolaire (QMS), un spectromètre laser (TLS) et de nombreux sous-systèmes.

Ces trois instruments sont intégrés dans une structure incluant l'échantillonneur de l'expérience constitué de 77 fours placés sur un carroussel. Ce système permet d'amener chacun des fours dans une position dans laquelle ils peuvent être remplis par des échantillons de sols ou de roches prélevés par Curiosity, puis de les amener une position dans laquelle il peuvent être chauffés jusqu'1100°C.Des échantillons d’atmosphère peuvent aussi être analysés. L’objectif principal reste l’analyse moléculaire du sol de Mars, en particulier dans le cadre de la recherche de composés organiques, volatils et réfractaires, ainsi que l’analyse isotopique et chirale.

Pour répondre aux objectifs scientifiques, SAM_GC est composé de six voies analytiques, chacune dédiée la séparation d'une gamme précise de composés potentiellement présents dans les échantillons analysés. Ces six voies incluent chacune une colonne chromatographique (tube capillaire) et un dispositif permettant de les maintenir température stable entre l'ambiante (environ 30°C) et 250°C. Cinq de ces voies sont équipées d’un détecteur autonome (nanoTCD). Consultation BDD

Mars2020 / SuperCam

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Sylvestre MAURICE [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUG Michel DIETRICH Lydie BONAL [email protected] OSUNA Thierry LE BEAU Nicolas MANGOLD [email protected] OVSQ Chantal CLAUD Franck MONTMESSIN [email protected] Obs. Paris Claude CATALA Thierry FOUCHET [email protected] OSUPS Nabila AGHANIM François POULET [email protected] OASU Marie Lise DUBERNET-TUCKEY Philippe PAILLOU [email protected]

Description

L’objectif de la mission Mars2020 est la recherche de traces d’une vie passée la surface de Mars, suite la découverte de l’habitabilité de Mars par la mission Curiosity. Lancée en juillet 2020, elle se posera sur la planète rouge en février 2021 et ses opérations se poursuivront, dans un premier temps, jusqu’en août 2023. Mars2020 consiste en un rover pourvu de nombreux instruments scientifiques, permettant de fournir des mesures de la surface de Mars ainsi que de préparer les futures missions de retour d’échantillons. L’instrument SuperCam a été conçu comme la continuité de l’instrument ChemCam, qui est un succès bord du robot Curiosity. En plus de la technique LIBS (“Laser-Induced Breakdown Spectrometry”) utilisée par ChemCam et permettant de connaitre la composition chimique de la cible, SuperCam utilisera la spectrométrie Raman ainsi que la spectrométrie infrarouge afin de connaitre la minéralogie des sols et roches la surface de Mars. Une caméra couleur donnera le contexte morphologique des mesures de chimie. L’objectif de SuperCam est de détecter des sources potentielles de bio-signatures (“PBS” - Potential BioSignatures), en combinant différentes techniques analytiques. SuperCam est constitué de trois parties: le “body unit”, localisé dans le corps du rover, le “mast unit” en haut du mât, et les cibles de calibration localisées sur le rover. Le Mast Unit est fourni par l’IRAP (co-PI S. Maurice) sous maitrise d’ouvrage CNES, alors que le Body Unit est fourni par le laboratoire de Los Alamos aux Etats-Unis (co-PI R. Wiens). L’université de Valladolid en Espagne est responsable du montage des cibles de calibration sur le rover, après leur fabrication en France. Consultation BDD

PLATO

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

PYTHEAS Bruno HAMELIN Magali DELEUIL [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA Marie-Jo GOUPIL [email protected] OSUPS Nabila AGHANIM Thierry APPOURCHAUX [email protected] Externe OSU : AIM Anne DECOURCHELLE Rafael GARCIA [email protected] OMP Michael TOPLIS Jérome BALLOT [email protected] Description

La mission PLAnetary Transits and Oscillations of stars, PLATO, est la mission M3 du programme Cosmic Vision (2015-2025) de l'ESA. PLATO, dont le tir est prévu en 2025, détectera et caractérisera des milliers d’exoplanètes de toutes tailles, dont plusieurs dizaines semblables la Terre, ainsi que leurs étoiles hôtes. L'atout de PLATO est que l’étude des transits planétaires sera non seulement couplée la sismologie de l’étoile hôte, mais aussi des mesures complémentaires réalisées par des spectrographes au sol. Chacune de ces méthodes permettant de mesurer des paramètres différents, il sera possible d'analyser avec précision les propriétés de ces systèmes. Différents laboratoires français contribuent de façon importante la réalisation de l'instrument mais surtout la préparation de la mission au niveau du centre de mission, le PLATO Data Center (PDC) et de la préparation scientifique (PSM). Les participations françaises concernant le système et la charge utile sont résumées ci-dessous: • Le LESIA (Observatoire de Paris) fournit: - le logiciel vol des N-DPU, - un rôle de conseil de niveau système instrument au sein du DPS, • Le CEA fournit: - un prototype numérique des F-FEE, • L’IAS (Orsay) assurera : - les essais thermiques d’étalonnage des caméras et la validation de leurs performances, ? En ce qui concerne le Centre de Données (PDC), les contributions françaises se déclinent comme suit:

- Pipeline L0 - L1: • le LESIA est responsable de l'étude et la définition des algorithmes de traitement de données bord et sol, ce qui inclut leur définition détaillée, et de la fourniture des logiciels pour la production de courbes de lumière prêtes pour les analyses scientifiques. • Le LESIA et l’IRAP participent au développement des procédures de test des différents modules du pipeline partir de données simulées

- Pipeline exoplanètes en charge produire les listes de transits et leurs caractéristiques : le LAM assure le développement et la fourniture de logiciels de détection, d’estimation des paramètres des systèmes planétaires et la gestion des performances de l’ensemble du pipeline

- Analyses stellaires: l'IAS est responsable du Système d'Analyses Stellaires (SAS) qui est chargé de la production et de la validation des paramètres stellaires dérivés partir des courbes de lumière L1 et des données auxiliaires (paramètres sismiques, paramètres relatifs l'activité stellaires, paramètres fondamentaux). Le CEA et l’IRAP contribuent certains WP.

- Outils en support aux analyses de données: le LAM est responsable du développement et de la fourniture des outils de contrôle des sorties du pipeline exoplanètes (visualisation, et outils de ré- analyse si nécessaire).

- Base de données ancillaire: le LAM est responsable de la définition et de la réalisation de la base de données qui va rassembler toutes les données auxiliaires, c’est dire autres que le catalogue d’entrée plus les données de suivi et les produits associés.

Le Plato Science Management assure le développement des méthodes et algorithmes, la préparation du catalogue d'entrée et identifie les besoins en termes de suivi sol. Il est placé sous la coordination Anglaise. Les responsabilités françaises sont réparties sur plusieurs types d’activités. Plus précisément:

- le LESIA porte la responsabilité générale de la préparation scientifique dans le domaine de la science conferences). physique stellaire;

- le LAM est responsable du développement des procédures pour établir la liste des priorités parmi les candidats planètes,

- L’IAS, le CEA, l’IRAP et le LUPM contribuent plusieurs aspects de la préparation en physique stellaire

- le CEA contribue également la préparation des activités pour l’analyse des interactions planète-étoile;

- l’OCA contribue l’élaboration du catalogue d’entrée et la fourniture de modèles de formation et d’évolution de planètes géantes.

- l’IPAG, l’IRAP, l’IAP et le LUPM contribuent certains aspects du follow-up que ce soit en physique stellaire ou sur la caractérisation des planètes.

Notons que seuls les WP du PSM jugés critiques pour le succès de la mission, c’est dire ceux qui sont indispensables pour fournir les produits PLATO sont soutenus financièrement par le CNES. Les autres correspondent des analyses scientifiques qui permettront d’optimiser le retour scientifique de la mission. Consultation BDD

Rosetta / CONSERT

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUG Michel DIETRICH Walter Wlodek KOFMAN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OVSQ Chantal CLAUD

Description

Philae a fonctionné pendant 64 heures de la séparation jusqu'l'hibernation. Consert a recueilli 50 minutes de données pendant la descente de Philae après la séparation, puis 9 heures de données de sondage travers la comète. L’interprétation scientifique continue. Actuellement, connaissant l’environnement de Philae après l’atterrissage, nous interprétons l’amplitude des signaux. Nous préparons aussi l’ensemble des données et de la documentation pour la base PSA. C’est un travail pour 2-3 ans, jusqu' fin 2018 où nous devrons fournir les données niveau L3. Consultation BDD

Rosetta / COSIMA

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUPS Nabila AGHANIM Yves LANGEVIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUC Yves COQUET Christelle BRIOIS [email protected]

Description

Ce service est dédié la contribution française l'expérience COSIMA sur l'orbiteur ROSETTA. Cette expérience sous responsabilité Allemande (Martin Hilchenbach, PI, MPPS Katlenburg Lindau) est dédiée l'analyse de grains collectés autour de la comète Churyumov-Gerasimenko par spectrométrie de masse temps de vol par émission d'ions secondaire (TOF-SIMS)

Contribution française : - microscope de détection des grains collectés (OSUPS/IAS) - canon ions (OSUC/LPCEE)

L'OSUPS intervient directement dans la définition de l'ensemble des séquences d'observations, car elles comportent systématiquement une utilisation de la caméra COSISCOPE, avec certaines séquences dédiées la caractérisation optique des grains: temps d'exposition, coordonnées de la cible pour l'obtention d'images résolution nominale ou sub-pixel (Nyquist), observations des grains collectés sous différents angles. l'OSUC intervient dans la définition des séquences d'observation comportant des analyses en masse en tant que responsable du canon ion. Il faut ajuster les paramètres des éléments de ce canon ion afin d'obtenir une résolution en masse et une intensité optimum des spectres Consultation BDD

Rosetta / MIRO

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Jacques CROVISIER [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

1- Génération de cartes de dégazage (zones d'activité) et de champs de vitesse du gaz pour contraindre les paramètres de la descente du lander et la sélection de son site d'atterrissage.

2 - Détermination des séquences d'observation et leur mise au point interactive en fonction des observations déjfaites, en utilisant nos modèles d'atmosphère cométaire.

3 - Établissement de catalogues de données de niveau 2 et de produits scientifiques.

4 - Mesure de constantes diélectriques de divers analogues d'astéroïdes et de noyaux cométaires pour l'interprétation des mesures de surfaces. Consultation BDD

Rosetta / OSIRIS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

PYTHEAS Bruno HAMELIN Laurent JORDA [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Ce service a pour but de réaliser: a) l'étalonnage en sol et en vol de l'instrument, b) le soutien aux opérations en vol, en particulier l'écriture de séquences d'observation pour envoi l'institut PI de l'instrument (MPS, Allemagne), et c) la préparation et la livraison de modèles en soutien aux opérations de la sonde et de l'atterrisseur PHILAE. Consultation BDD

Rosetta / VIRTIS

Type

AA-ANO2

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Stéphane ERARD [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Fonctionnement de l'expérience VIRTIS bord de la sonde Rosetta : - Préparation de la stratégie d'observation en orbite cométaire et implémentation. - Opérations la comète - Suivi de l'instrument en vol - Réception, gestion et calibration des données de la voie H - Fourniture et maintenance du logiciel de lecture/écriture des données - Calculs des données géométriques pour les deux voies M et H - Documentation de l'archive PSA/ESA. Consultation BDD

ALMA Regional Center

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OASU Marie Lise DUBERNET-TUCKEY Stéphane GUILLOTEAU [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Externe OSU : IRAM Karl SCHUSTER Frédéric GUETH [email protected] OSUG Michel DIETRICH Jean-Charles AUGEREAU [email protected] Obs. Paris Claude CATALA Darek LIS [email protected]

Description

Le ALMA Regional Center (ARC) est en charge de tous les aspects liés au fonctionnement scientifique de ALMA en Europe. L'ESO porte la responsabilité principale (gestion des programmes d’observation, archivage des données, etc.) mais est épaulé par un réseau de sept instituts européens, appelés “noeuds”. L’IRAM fait partie de ce réseau. Ses tâches comprennent essentiellement :

• aide aux utilisateurs pour la validation des scheduling blocks des projets acceptés ; • support aux utilisateurs pour la réduction de données, notamment lors de visites l’IRAM ; • développement de logiciels et de scripts de réduction de données.

Le noeud de l'ARC l'IRAM s'adresse aux communautés françaises, allemandes et espagnoles (les trois pays partenaires de l’IRAM). Consultation BDD

CFHT

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Externe OSU : INSU Guy PERRIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Situé 4200 m d’altitude au sommet du Mauna Kea Hawaii, le télescope CFHTde 3,60 m de diamètre offre la communauté scientifiqueune caméra optique grand champ (MegaCam), une caméra grand champ infrarouge (WIRCam) et un spectropolarimètre échelle haute résolution (ESPaDOnS). D’autres instruments sont en développement. La société du CFHT est une organisation gérée conjointement par le NRC (Canada), le CNRS (France) et l’Université d’Hawaii. Le personnel scientifiquedu CFHT est composé d'astronomes résidents, d'astronomes visiteurs, des observateurs de service et des assistants l’observation. Consultation BDD

IRAM

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OASU Marie Lise DUBERNET-TUCKEY Stéphane GUILLOTEAU [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Externe OSU : IRAM Karl SCHUSTER Frédéric GUETH [email protected] OSUG Michel DIETRICH Jean-Charles AUGEREAU [email protected] Obs. Paris Claude CATALA Darek LIS [email protected]

Description

Soutien aux instruments des deux observatoires de l’IRAM : l’interféromètre du Plateau de Bure et le télescope de 30-mètres Pico Veleta. En particulier: - développement et commissioning de NOEMA - développement et commissioning de nouvelles instrumentations, en particulier la caméra continuum NIKA2 Consultation BDD

LOFAR-NenuFAR

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUC Yves COQUET Jean-Mathias GRIESSMEIER [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA OCA Thierry LANZ Chiara FERRARI [email protected] OSUPS Nabila AGHANIM

Description

La station LOFAR-FR606 fait partie d’un réseau l’échelle européenne. Au total, ce réseau regroupe actuellement 51 stations réparties en 7 pays. LOFAR connaît deux modes d’opération: • le mode «international», dans lequel les données de chaque station sont acheminées au corrélateur central aux Pays-Bas, • le mode «local» ou «stand-alone», dans lequel les stations internationales fonctionnent comme des observatoires indépendants.

NenuFAR a été concu comme une extension de la station LOFAR Nancay, avec une sensibilité largement augmentée (plus d’un ordre de grandeur), notamment pour les plus basses fréquences (<30 MHz). De la même manière que la station LOFAR-FR606, NenuFAR fonctionne en deux modes différents: • le mode «super-station», ou les antennes NenuFAR sont intégrées au réseau LOFAR au lieu des antennes LOFAR-FR606. • le mode «independent», ou NenuFAR est opéré comme instrument indépendant.

Dans le cadre du service national d’observation, il s’agit de d’opérer et exploiter LOFAR-FR606 et NenuFAR et de consulter et aider les utilisateurs pour maximiser le retour scientifique. Consultation BDD

Observatoires au Chili (ESO La Silla, ESO Paranal, ALMA Chajnantor, APEX)

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Externe OSU : INSU Guy PERRIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Externe OSU : AIM Anne DECOURCHELLE Philippe ANDRÉ [email protected] IAP Francis BERNARDEAU Hélène ROUSSEL [email protected]

Description

L’ESO (European Southern Observatory) gère trois sites d'observation de classe internationale répartis dans la région chilienne du désert d'Atacama: La Silla,Paranalet Chajnantor. Le site de La Silla, 2400 m d’altitude, offre plusieurs télescopes dont le 3,60 m,équipé du spectrographe haute résolution HARPS, et le NTT. Le site deParanal, 2600 m d’altitude, abrite le VLT constitué de 4 télescopes de 8,2 m de diamètre, de 4 télescopes auxiliaires mobiles permettant un fonctionnement en mode interférométrique (VLTI), le tout étant équipé de plus d’une dizaine d’instruments. Sur le plateau de Chajnantor plus de 5000 m d'altitude, ALMA (Atacama Large Millimeter/submillimeter Array) est un réseau de 66 antennes permettant des observations dans le domaine millimétrique et sub-millimétrique avec des lignes de base pouvant atteindre 16 km. ALMA est un observatoire développé etexploitéconjointement par l’ESO, la NSF (Etats-Unis), le NINS (Japon) en coopération avec le Chili.Enfin, l'ESO exploite également, sur le plateau de Chajnantor, APEX (Atacama Pathfinder Experiment), un télescope de 12 mètres de diamètre observant dans les longueurs d'ondes millimétrique et submillimétrique (Le SNO comprend le travail de suivi de la caméra ArTéMiS sur le ciel avec mise disposition des données calibrées). La France contribue directement l’ESO hauteur de 17% et indirectement via la construction d’instruments et une contribution aux développements d’infrastructures. Consultation BDD

Radiotélescope décimétrique de Nançay

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Gilles THEUREAU [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUC Yves COQUET

Description

Le grand Radiotélescope décimétrique de Nançay est la 4ème antenne unique au monde. Sa dernière rénovation majeure date de 2000 (projet FORT), quand les instruments d'analyse (spectrographes, traitement des interférences, dédisperseur cohérent pulsars) ont été constamment remis jour depuis. Cet instrument national est ouvert la communauté internationale via un appel propositions semestriel, géré par un comité des programmes formé de membres des programmes nationaux (PNCG, PNHE, PNPS, PNP), d'un membre de RADIONET/FP7, avec l'appui d'un groupe d'experts internationaux. L'instrument fonctionne 24h/24, 7j/7, 365j/an. Le service comprend l'encadrement scientifique des développements instrumentaux pour de nouvelles générations de backends, le suivi de la calibration/polarisation et de la qualité des données, le développement et l'évolution des logiciels de traitement des données et leur mise disposition aux utilisateurs, la formation des utilisateurs, la coordination des campagnes de tests, la mise en oeuvre du planning des observations, la coordination et la mise en oeuvre de la maintenance de jouvence de l'instrument (informatique, mécanique-électrotechnique, électronique et performances instrumentales). Consultation BDD

SUV (Service aux Utilisateurs du VLTI)

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OCA Thierry LANZ Alexis MATTER [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUG Michel DIETRICH Jean-Charles AUGEREAU [email protected] Obs. Paris Claude CATALA Vincent COUDE DU FORESTO [email protected] OSUL Isabelle DANIEL Eric THIEBAUT [email protected]

Description

En tant que nouveau service du pôle thématique national JMMC, le SUV (Service aux Utilisateurs du VLTI) assure, au sein des observatoires concernés (Nice, Grenoble, Paris, Lyon), un service de support aux utilisateurs des instruments de deuxième génération du VLTI. Il se traduit par une assistance personnalisée (questions, assistance face face) la préparation des propositions d'observation et des observations, et au traitement des données des instruments GRAVITY et MATISSE. Cela inclut également une assistance dans l'utilisation critique des logiciels de reconstruction d’image et d’ajustement de modèle du JMMC. Vis vis du JMMC/MOIO et de l’ESO, il est également prévu une implication forte dans le maintien et le développement des pipelines de réduction de données grâce au retour des utilisateurs et des personnels du SUV. Consultation BDD

Télescope Bernard Lyot au Pic du Midi

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Éric JOSSELIN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

La mission du Télescope Bernard Lyot est de produire des données astronomiques pour la communauté en maintenant le télescope et son instrumentation en phase avec les demandes. Le TBL/Narval occupe une niche en magnétisme stellaire depuis 2007. Le TBL offre un service d'observation complet de la gestion des demandes la publication des données (observations de services, controle qualité, réduction des données). 15 agents (8 CNRS, 7 Univ de Toulouse Paul Sabatier) sont requis et un responsable scientifique. L'équipe scientifique d'observation de service demande 4 ETP de tache de service CNAP réparties en une vingtaine d'observateurs par an. Coût 150 k€ fonctionnement, 800 k€ de salaires. Consultation BDD

Télescope de 193 cm de l'OHP

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

PYTHEAS Bruno HAMELIN Auguste LE VAN SUU [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Station d’observation de l’OHP avec le télescope de 193cm. Mise disposition T193+SOPHIE, possibilité d'y opérer des instruments visiteurs comme GHASP, MYOSOTIS ou tout autre instrument au foyer Cassegrain du T193. Ce service d'observation sert la communauté astronomique Française des programmes nationaux et des programmes Européens Opticon (10 nuits/semestre) Consultation BDD

THEMIS

Type

AA-ANO3

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Externe OSU : THEMIS Bernard GELLY Bernard GELLY [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Télescope solaire optique de 1m implanté Ténérife, spécialisé en spectropolarimétrie solaire, cartographie du champ magnétique, étude des processus d'émergence du flux magnétique et transport vers la chromosphère. Nons offrons également des possibiltés d'observations planétaires, et en particulier Mercure. Consultation BDD

CHEOPS

Type

AA-ANO4

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

PYTHEAS Bruno HAMELIN Magali DELEUIL [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Description

Les activités liées la préparation de l’instrument pour la participation française sont concentrées sur le segment sol de la mission et plus particulièrement sur la chaîne de traitement des données avec production des courbes de lumière prêtes pour les analyses scientifiques). La participation française inclut également la contribution l’élaboration du catalogue d’entrée de la mission.

1. Elaboration de la chaîne de traitement N1-N2 des données CHEOPS (WP#10): Le Centre d’opération et de traitement des données est sous responsabilité suisse. Il sera installé et opéré Genève. La Figure 2 présente l’organigramme du SOC. La contribution française porte sur le “Workpackage” numéro 10 (WP #10), en charge du traitement des données et dont le LAM a la responsabilité française et auquel contribue également le CAUP (Portugal). L’objectif est de concevoir et réaliser la chaîne de traitement qui, partir de la série d’images brutes que délivrera l’instrument, fournira des courbes de lumières calibrées et prêtes pour les analyses scientifiques. La difficulté consiste extraire la photométrie avec la meilleure précision possible dans les conditions d’observation propres CHEOPS, et en tenant compte de configurations stellaires particulières qui peuvent affecter la précision photométrique (contaminants proches). Les algorithmes de ce logiciel seront développés et mis au point partir d’images simulées fournies par un outil opérationnel qui simule les images théoriques attendues (CHEOPSSim) en tenant compte de l’optique et des conditions d’observation. Le logiciel est en cours de réalisation en conformité avec le cahier de charge du SOC en terme de langage de programmation, d’infrastructure et d’interfaces. La chaîne de traitement respecte les interfaces avec les autres “workpackages” notamment ceux en charge du pré-traitement et des archives. Il est développé au LAM au CESAM et déployé dans le centre mission (Science Operation Center) qui est Genève. En tant qu’outil opérationnel, la chaîne sera suivie pendant les opérations et les algorithmes seront mis jour partir des données réelles. Sur le plus long terme, le LAM est responsable de la fourniture des logiciels de correction des effets de vieillissement de l’instrument.

2. Participation au catalogue d’entrée : L’expertise de la communauté française en matière d’exoplanètes et en particulier dans le domaine des vitesse radiale est sollicitée pour préparer le catalogue d’entrée en collaboration avec le consortium. La mission CHEOPS est en effet une mission dite “de suivi” qui observera des étoiles pour lesquelles les grands relevés vitesse radiale ou les relevés photométriques au sol de nouvelle génération (NGTS) auront déjrévélé la présence d’une planète. Il conviendra donc de sélectionner les meilleures cibles de façon optimiser la programmation des observations. Ce travail sera basé sur les résultats des campagnes de mesures de vitesse radiale avec des spectrographes mais aussi sur des recherches partir des grandes bases de données nationales. Il pourra également nécessiter des observations préparatoires spécifiques. Dans notre participation au catalogue d'entrée, l'apport de catalogue de sources avec vitesses radiales mesurées est sous la responsabilité du LAM Consultation BDD

Centre de Données astronomiques de Strasbourg (CDS)

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

ObAS Pierre-Alain DUC Mark ALLEN [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Le Centre de Données astronomiques de Strasbourg est dédié la collecte et la distribution de données astronomiques. Il fournit la communauté scientifique internationale des services haute valeur ajoutée, principalement SIMBAD, la base de référence pour la nomenclature et la bibliographie des objets astronomiques, VizieR, le service de référence pour les catalogues astronomiques et les tables publiées dans les journaux académiques de la discipline, qui comprend de plus en plus de données autres que des tables "attachées aux publications" (images, spectres, séries temporelles), le CDS X-match, le service de corrélation croisée des grandes catalogues astronomiques. Aladin et Aladin-Lite atlas interactif du ciel qui est le portail images de l'observatoire virtuel, en particulier les données HiPS (Heirarchical Progressive Surveys). Aussi un Dictionnaire de Nomenclature des objets astronomiques (hors système solaire). Outre la maintenance des services, les activités du CDS comprennent une activité soutenue de R&D, essentielle la pérennité sur le long terme du Centre de Données, des collaborations avec les archives des télescopes sol et spatiaux, ADS et NED, et les journaux académiques de la discipline, et il joue un rôle important, au niveau national, européen et international, dans le développement de l'Observatoire Virtuel astronomique. Consultation BDD

APIS

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Laurent LAMY [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

The Auroral Planetary Imaging and Spectroscopy (APIS) service accessible at http://apis.obspm.fr provides an open and interactive access to processed auroral observations of the outer planets and their satellites. Such observations diagnose powerful electromagnetic emissions radiated around the magnetic poles of giant planets of the solar system, as a result of the interaction between the magnetosphere, the upper atmosphere, the moons/rings and the solar wind. These data are therefire of interest for a wide community at the interface between planetology, magnetospheric and heliospheric physics. APIS consists of (i) a high level database archived at VO-Paris Data Centre, built from planetary auroral observations acquired by the Hubble Space Telescope (HST) since 1997 with its mostly used Far-Ultraviolet spectro-imagers, (ii) a dedicated search interface aimed at browsing efficiently this database through relevant conditional search criteria and (iii) the ability to interactively work with the data online through plotting tools developed by the Virtual Observatory (VO) community, such as Aladin and Specview, through the SAMP protocol. This service is VO compliant and can therefore also been queried by external search tools of the VO community (such as VESPA, CDPP/AMDA, HELIO etc.). The diversity of available data and the capability to sort them out by relevant physical criteria shall in particular facilitate statistical studies, on long-term scales and/or multi-instrumental combined analysis. Fortuitously, APIS is also the ancient egyptian god of (data) fertilization. Consultation BDD

Encyclopédie des planètes extrasolaires

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Françoise ROQUES [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Le portail exoplanet.eu de l’Encyclopédie des Planètes Extrasolaires comprend - une base de données des exoplanètes connues (6,000 planètes confirmées et candidates) et des étoiles associées - différents outils d’analyse - une bibliographie associée (16,500 titres) - une listes des colloques - une liste des instruments sol/espace - des liens avec les principaux sites du domaine. L’ajout de nouvelles fonctionnalités est en cours. Le contenu est décrit dans Schneider et al. A&A 532 A79, 2011. Une collaboration se met en place avec le Data and Analysis Center for Exoplanets de l’université de Genève, membre du consortium PlanetS. Consultation BDD

VESPA

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Stéphane ERARD [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

Le Portail VESPA fournit un accès unifié aux bases de données pour l'étude du Système Solaire, ainsi qu'un système de fouille de ces bases de données et de visualisation performant. La valeur ajoutée consiste en la fourniture d'un accès immédiat depuis une interface unique tous les services utilisant le protocole EPN-TAP, et en des fonctions standard de visualisation et de traitement en ligne. Il permet notamment la fouille de données croisée entre différents services. - L’interface VESPA permet de fouiller le contenu des bases de données partir de critères observationnels ayant un sens physique. L’ensemble des services connectés est interrogé simultanément. Pour chaque service, le résultat d’une recherche est la liste des fichiers remplissant les conditions indiquées. - La connexion des outils OV sur l’interface permet la lecture et la visualisation en ligne des fichiers sélectionnés dans la plupart des cas (images, spectres, séries temporelles, profils, cubes spectraux, etc.). - Ces mêmes outils fournissent également des capacités de traitement standard en mode interactif. - L’interrogation simultanée permet déjde croiser des observations similaires, par exemple des observations coordonnées de plusieurs instruments ou sondes spatiales. A terme, l’interface permettra d’effectuer des interrogations plus complexes entre services (utiliser les résultats d’une recherche pour déterminer les paramètres de la recherche suivante).

Les bases de données accessibles incluent des services de référence labellisés aussi bien que des bases de données thématiques de taille variée (par ex. archive planétaire de l'ESA, en cours). Il est également ouvert aux contributeurs scientifiques, le système étant facile mettre en place par une petite équipe. Le nombre de services de données accessibles et d’outils de traitement disponibles sont augmentés dans le cadre du programme Europlanet H2020. Ce programme fournit également un support aux fournisseurs de données et aux utilisateurs. Consultation BDD

VO Solar System Objects Portal

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

IMCCE Jacques LASKAR Jérôme BERTHIER [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA William THUILLOT [email protected]

Description

Le portail VO-SSO regroupe un ensemble de services et de bases de données dédiés aux corps du système solaire dans le cadre de l'Observatoire Virtuel. Il met la disposition de la communauté astronomique professionnelle et amateur, le grand public et le monde de l’éducation toute l'expertise de l'IMCCE en science planétaire. Le portail VO-SSO s’articule autour de trois axes : l’information, les éphémérides et l’observation astronomique des corps du système solaire, au travers de quatre grands services (Skybot, Miriade, M4AST, SsODNet). Le portail intègre le centre d'expertise PADC. Consultation BDD

F-VAMDC

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Marie-Lise DUBERNET [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU THETA OASU Description

"F-VAMDC" est un service du "Pôle Thématique Diffusion Physique Atomique et Moléculaire" et est partenaire du consortium international VAMDC. "F-VAMDC" s'engage suivre la charte du consortium international VAMDC afin de pouvoir prétendre une appellation "VAMDC". VAMDC permet une interrogation croisée d'un ensemble de bases de données dont 90% sont utilisées en astrophysique avec un format unique pour récupérer des données. Les fichiers récupérés peuvent être exploités travers le portail VAMDC et travers des outils logiciels développés dans VAMDC ou bien par des tiers. Je renvoie l'évaluateur vers les success stories (http://www.vamdc.org/news/success-stories/). A noter que certaines bases comme HITRAN, JPL, CDMS, les bases de Dijon (http://vamdc.icb.cnrs.fr/PHP/methane.php, http://vamdc.icb.cnrs.fr/PHP/shecasda.php, http://vamdc.icb.cnrs.fr/PHP/tfmecasda.php), de Reims (http://vamdc.univ-reims.fr/PHP/ethylene.php, http://smpo.univ-reims.fr/), de l'OSU THETA ont des données qui intéressent aussi la partie OA de l'INSU.

"F-VAMDC" a plusieurs activités de service : 1. La maintenance et l’évolution des standards qui caractérisent le langage commun d’interopérabilité (langage d’interrogation, mots clés/vocabulaire/sémantique, « format/structure » des informations renvoyées par les bases de données) et des « registries » (http://vamdc.eu/standards). Ceci inclut le travail d'interoperabilité avec l'IVOA en cours. (OBSPM, OSU THETA, OASU) 2. La maintenance et les mises jour des logiciels communs tels que les suites logicielles implémentant au niveau des bases de données les standards définis ci-dessus (Node Software En Java, – http://vamdc.eu/software), le logiciel TAPValidator permettant de tester la qualité des services (– http://vamdc.eu/software), les supports aux utilisateurs (OBSPM, OSU THETA) 3. La maintenance et les mises jour, voire les développements des briques de l'infrastructure VAMDC comme les "registries". Sans les registries il est impossible aux applications telles que le portail, les outils d'analyse comme CASSIS ou SPECTCOL de trouver les ressources de l'infrastructure VAMDC (OBSPM) 4. La maintenance et le upgrade de la "species database". Cette base de données s'update automatiquement avec les nouvelles espèces rajoutées dans les bases de données, et exposées dans VAMDC. Cette base est centrale pour interoperabilité des recherches par espèces chimiques sur 30 bases de données ce qui est assez unique. Cette "species database" requiert de l'attention et la mise en place de services supplémentaires de temps en temps (OBSPM, OSU THETA, OASU) 5. La maintenance et l'évolution du portail VAMDC qui donne accès toutes les bases de données connectées VAMDC (http://portal.vamdc.eu). Ce portail utilise l'ensemble des éléments 1, 2, 3 ci-dessus et inclut des processeurs de visualisation de données. Le portail donne accès aux données via le langage natif XSAMS, les fichiers peuvent être téléchargées et re-exploitées en local pour de l'inter-comparaison de données provenant de bases de données différentes (OBSPM) 6. La vérification de la qualité des données qui sont distribuées dans VAMDC par les bases de données connectées. Cette vérification s'effectue avec TAPValidator pour le format des fichiers, via le portail VAMDC, via les outils logiciels applicatifs comme SPECTCOL (OBSPM) 7. La maintenance et les mises jour des logiciels applicatifs, dont le but est de rendre un service une communauté d’utilisateurs : le logiciel SPECTCOL pour la manipulation conjointe de données de spectroscopie et de collisions (http://vamdc.eu/software). Le logiciel SPECTCOL est utilisé par CASSIS pour remplir sa propre base de données interne, et également par le groupe de Peter Schilke pour CASA (ALMA). Ce logiciel a permis un récupération sans effort de la totalité de la base BASECOL des fins d'utilisation pour ces logiciels (OBSPM) 8. La création de nouveaux logiciels/outils/processeurs pour des utilisateurs précis. Ces outils vont manipuler les données issues de l’infrastructure pour une application très précise. le dernier exemple est la création par le groupe de l'OSU THETA de processeurs permettant d’extraire l’ensemble des données de spectroscopie moléculaire au format HITRAN (très largement utilisé par l’ensemble de la communauté « moléculaire », par les codes de transfert radiatif, etc. ; d’autres formats sont venir). Il est ainsi désormais possible d'analyser conjointement et de comparer, par exemple, des données HITRAN et JPL/CDMS (et d’autres) ce qui est impossible faire sans l'infrastructure VAMDC 9. La maintenance et les mises jour locales des bases de données qui doivent soit faire des mises jour de leurs « logiciels maisons » qui implémentent les standards VAMDC, soit récupérer le logiciel « Node Software » et coder les quelques lignes permettant de l’adapter la base locale. Pour Observatoire de Paris : BASECOL, Stark-B, TipTopBAse, Sesam; pour OASU : KIDA, pour OSU THETA : (http://vamdc.icb.cnrs.fr/PHP/methane.php, http://vamdc.icb.cnrs.fr/PHP/gecasda.php, http://vamdc.icb.cnrs.fr/PHP/rucasda.php , http://vamdc.icb.cnrs.fr/PHP/tfmecasda.php, http://vamdc.icb.cnrs.fr/PHP/shecasda.php) 10. La coordination politique, scientifique et technique du Consortium International VAMDC et la participation au board de VAMDC (OBSPM, OSU THETA, OASU) 10. Le support aux utilisateurs (OBSPM) 11. La réplication des services de VAMDC (OBSPM) 12. Le monitoring des services de VAMDC (OBSPM) 13. Le développement R&D qui va plus loin que l'infrastructure VAMDC créé dans le cadre des projets européens FP7 VAMDC et F-VAMDC. Cela concerne les travaux sur la citation de données au niveau international du "Research Data Alliance" avec l'implémentation des concepts développés travers un Query Store (http://www.vamdc.org/type_successstories/vamdc-query-store/), et la continuité de ces travaux vers la notion de DO (Digital Object dans le cadre EU) (OBSPM). 14. Le développement R&D nécessaire pour manipuler de très gros volumes de données. Travail en réflexion. Consultation BDD

MP3C

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OCA Thierry LANZ Marco DELBO [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

MP3C (Minor Planet Physical Properties Catalogue) est une base de données relationnelle de propriétés physiques et dynamiques d’astéroïdes, née d’une initiative de M. Delbo’ et P. Tanga (équipe de Théorie et observation en Planétologie, TOP, Laboratoire Lagrange, OCA) pour répondre d’une façon efficace aux besoins de la communauté qui étudie les petits corps du Système Solaire, en France et l’étranger. Le but de ce service est de réunir dans une seule interface l’accès aux données dynamiques et physiques de ces objets, aujourd’hui dispersées dans une variété de bases très différentes, parfois avec des formats arbitraires. La valeur ajoutée de MP3C consiste en la possibilité d’effectuer des opérations d'algèbre relationnelle telles que l'intersection, la sélection et la jointure sur la base de données grâce un moteur SQL. Par exemple, MP3C permet de sélectionner tous les astéroïdes dans un certain intervalle de paramètres orbitaux avec un certain albédo et/ou couleur. MP3C est le premier et unique service qui permet d’accéder aux données des petits corps avec des standards propres l’Observatoire Virtuel. Consultation BDD

SPHERE Data Centre

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUG Michel DIETRICH Nadège MEUNIER [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OCA Thierry LANZ [email protected] PYTHEAS Bruno HAMELIN Hervé LE COROLLER [email protected] Obs. Paris Claude CATALA Raphaël GALICHER [email protected]

Description

Le centre de données SPHERE est un centre de traitement de données la demande entré en opération début 2015, lors de l’entrée en fonction de SPHERE Paranal. Il s’adresse tous les PI d’observation SPHERE en leur proposant de réduire leurs données SPHERE. L’objectif est d’optimiser le retour scientifique sur l’instrument, dans un contexte très compétitif et de besoin d’une forte valeur ajoutée lorsque l’on utilise des outils optimisés haut contraste – que ne fournit pas l’actuel pipeline de l’ESO. Les données publiques sont également réduites par le centre de données pour mise disposition publique. Une partie de nos services vise un public d’observateurs non spécialistes de l’instrument, en leur apportant une expertise forte. En effet, du fait de la complexité de l’instrument et du nombre de modes observationnels disponibles, il peut être difficile pour des collègues non spécialistes de ce type de données de les exploiter complètement. Ceci est particulièrement vrai pour des collègues spécialistes d’autres techniques (par exemple vitesses radiales) s’intéressant des observations effectuées avec des instruments complémentaires. D’autres services s’adressent plutôt des observateurs ayant une bonne connaissance de l’instrument, en leur fournissant une infrastructure, des outils et une logistique leur permettant une réduction efficace de leurs données. Dans le cadre de grands relevés, il est par exemple crucial d’assurer sur le long terme un traitement homogène afin de garantir l’exploitation statistique des résultats. Dans ce cas il s’agit de faire une partie du traitement la demande mais aussi de fournir des outils permettant une réduction efficace et homogène. L’équipe du centre de données va également ensuite assurer un suivi sur le long terme des performances de l’instrument en collaboration étroite avec l’ESO, certaines informations pertinentes provenant en effet des données scientifiques alors que d’autres sont extraites des mesures obtenues lors des activités de maintenance Paranal (activité de nature SO2). Enfin, le centre de données joue également un rôle moteur dans l’évolution des routines de traitement de ces données qui permettra une amélioration du pipeline qui profitera tous les utilisateurs (via le centre de données) et un retraitement des données avec ces nouvelles routines. Consultation BDD

SSHADE-F-GhoSST

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUG Michel DIETRICH Bernard SCHMITT [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUPS Nabila AGHANIM Rosario BRUNETTO [email protected] OMP Michael TOPLIS Patrick PINET [email protected] OSUNA Thierry LE BEAU Marion MASSÉ [email protected] Description

SSHADE-F "Solid Spectroscopy Hosting Architecture of Databases and Expertise" GhoSST “Grenoble Astrophysics and Planetology Solid Spectroscopy and Thermodynamics" database service

* Thématique concernée : SSHADE est une infrastructure interopérable de bases de données spectroscopiques des solides couvrant tout le domaine électromagnétique, des rayonnements gamma aux ondes radio, en passant par les rayonnements X, UV, visible, infrarouge et millimétrique. Les solides naturels ou synthétiques concernés sont issus d'expériences de laboratoire, d'analogues terrestres ou de cosmo-matériaux (glaces, minéraux, matériaux organiques et inorganiques, (micro-)météorites, IDPs, matériaux optiques, …). Elle fournit, via une série de bases (GhoSST, DAYSY, FAME, PaSSTEL, STOPCODA, SSTONE, MIA, BYPASS, DOCCD, LSD, SOSYPOL), les données de laboratoire ou de terrain, ainsi que les produits dérivés indispensables l’analyse et la modélisation des très nombreuses données d’observations spectroscopiques (de l'UV au mm) des surfaces et atmosphères (aérosols, nuages, poussières, …) des planètes, Terre incluse, et des autres objets du système solaire (satellites, astéroïdes, comètes, …) ainsi que des grains interstellaires et circumstellaires, issues des missions spatiales et des télescopes au sol. Elles servent aussi l’interprétation d’analyses de cosmo-matériaux, de simulations expérimentales et de mesures terrain.

* Contexte du SO Le service SSHADE-F-GhoSST (https://www.sshade.eu), issu par extension (en décembre 2017) du service GhoSST labélisé en janvier 2013 (https://ghosst.osug.fr), consiste en la mise en place et l’alimentation d’une série de bases de données sur les propriétés spectroscopiques des solides d’intérêts planétologique et astrophysique, mais aussi terrestre. L'infrastructure SSHADE est basée sur le modèle de données SSDM (Solid Spectroscopy Data Model) que nous avons spécialement développé pour ce domaine depuis 2006. Les données de la base GhoSST sont issues de diverses expériences de laboratoire effectuées sur une grande variété de solides depuis 1989, au LGGE, puis au LPG, et actuellement l’IPAG (équipe de planétologie). Le contenu des autres bases est issu soit de données publiées, ou non, mais non diffusées, soit de données déjdiffusées via des pages web (comme la base DOCCD de Jena).

* Organisation locale, nationale et internationale : SSHADE regroupe actuellement 11 bases de données de 4 pays (F, D, PL, CH) dont 7 par des équipes de recherche de 6 laboratoires français, sur 4 OSUs (OSUG, OSUNA, OMP et OSUPS). A court terme (2019) elle s'étendra 21 équipes de recherche de 10 pays, principalement européens (F, I, D, GB, E, CH, PL, HU, IN, TW) (cf. http://wiki.sshade.eu/) dont 10 bases de données de 9 laboratoires français, sur 7 OSUs.

Les 6 bases françaises actuellement directement concernées par le service sont: - GhoSST: “Grenoble Astrophysics and Planetology Solid Spectroscopy and Thermodynamics" database service, Planeto/IPAG, Grenoble (OSUG) - DAYSY: Database for AstrochemistrY and SpectroscopY, Astrochimie et Origines/IAS, Orsay (OSUPS) - FAME: French Absorption spectroscopy beamline in Material and Environmental science database service, FAME/ESRF, Grenoble (OSUG) - PaSSTEL: PlanetAry Surface Spectroscopy Toulouse Experimental Laboratory, PEPS/IRAP, Toulouse (OMP) - STOPCODA: Database for SpecTroscopy and Optical Properties of Cosmic Dust Analogues, MICMAC/IRAP, Toulouse (OMP) - SSTONE: Solid Spectroscopy daTabase Of NantEs, Surfaces planétaires & Intérieurs planétaires/LPGN, Nantes (OSUNA)

SSHADE et GhoSST, la base de donnée 'historique' (https://ghosst.osug.fr) et actuellement la plus fournie en données, font partie du centre d’expertise régional OSUG-DC (OSUG Data Center) et sont aussi liés VESPA (Virtual European Solar and Planetary Access) et au centre thématique F-VAMDC (Virtual Atomic and Molecular Data Center).

SSHADE est en développement dans le cadre du programme H2020 "Europlanet 2020-RI". L'infrastructure avec 11 bases a été livrée l'Europe, et ouvert au public le 1er Février 2018 (https://www.sshade.eu). Elle continue son extension en nombre de bases et en contenu, mais aussi en type de données (ajout d'une 'liste de bandes', ...) et en outils pour les utilisateurs via son interface.

* Liste des tâches relevant du SO SSHADE-F-GhoSST - Appui au développement du modèle de données SSDM et de l'interface de SSHADE - Alimentation de la base commune de SSHADE en données fondamentales - Compilation critique de données et alimentation de la base de « liste de bandes » des solides moléculaires - Formation des ‘scientific managers’ et ‘database managers’ des bases de données de SSHADE - Documentation, préparation, validation et ingestion de données dans la base de données GhoSST, et dans les autres bases d'OSUs (DAYSY, FAME, PaSSTEL, STOPCODA, SSTONE) - Support aux fournisseurs de données Européens - Formation et support aux utilisateurs de SSHADE - Animation scientifique de la base Consultation BDD

Méthodes et Outils pour l'Interférométrie Optique

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUG Michel DIETRICH Gilles DUVERT [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OCA Thierry LANZ Armando DOMICIANO [email protected] OSUL Isabelle DANIEL Eric THIEBAUT [email protected] Obs. Paris Claude CATALA Description

Le SNO MOIO est, au sein du Pôle Thématique National JMMC, chargé de la création, suivi et maintenance des logiciels nécessaires une utilisation optimale des interféromètres optiques ouverts la communauté, notamment le VLTI de l'ESO, avec les instruments AMBER, PIONIER, GRAVITY et MATISSE, mais aussi l'interféromètre CHARA avec l'instrument VEGA.

Ces logiciels sont la vitrine de l'expertise nationale en interférométrie optique, portée par plusieurs dizaines de chercheurs dans les laboratoires des 4 OSUs partenaires et de l'ONERA. Rassemblée en réseau de R&D au sein de MOIO, cette expertise a conduit la coréalisation, par les chercheurs et les ingénieurs du SNO, d'un éventail complet de logiciels et services web permettant de faciliter la vie des spécialistes mais aussi des non-spécialistes:

- La préparation des observations interférométriques: ASPRO; GetStar; SearchCal... - L'observation en mode visiteur et/ou déléguée: ASPRO - La normalisation du format OIFITS d'échange de données interférométriques; OIVal - La réduction de données: AMBER et PIONIER, terme les instruments de 2eme génération du VLTI. - La visualisation de données: OIFitsExplorer - L'analyse des résultats, que ce soit pour l'ajustement de modèles (LITpro) ou la reconstruction d'image (OImaging, WISARD) - Les bases de données nécessaires pour l'interférométrie optique (JMDC, JSDC pour les diamètres stellaires, BadCal...) - Le portail d'entrée mondial des observations d'interférométrie optique: la base de données OIdB.

L'ensemble des logiciels existant et en préparation se répartit sur les quatre groupes d'intérêt qui constituent MOIO (voir organigramme).

Ces logiciels sont en particulier utilisés dans le deuxième SNO du JMMC, le SNO3 SUV, dans ses actions de support aux utilisateurs et de formation. Concus pour être universels, ils sont utilisés partout dans le monde ou des chercheurs font des observations en interférométrie optique. Le retour sur citation (remerciements au JMMC sur tel ou tel logiciel) atteint 70% des publications de rang A de la dicipline.

Les actions et logiciels de MOIO sont disponibles et documentés sur htpp://www.jmmc.fr Le pôle JMMC est doté d'un conseil scientifique qui examine annuellement le rapport d'activité de MOIO (disponible sous http://www.jmmc.fr/doc/index.php?type=TRE ), valide les actions en cours et peut définir de nouvelles tâches de service (voir http://www.jmmc.fr/job_offers.htm)

MOIO est ainsi un mini-CDS pour l'interférométrie optique. CDS avec qui il partage un attachement particulier l'Observatoire Virtuel. Consultation BDD

PSuP

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUPS Nabila AGHANIM François POULET [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUL Isabelle DANIEL Cathy QUANTIN-NATAF [email protected]

Description

PSuP (Portail des SUrfaces Planétaires) consiste en un centre de traitement de données de surfaces planétaires couplé un centre de diffusion et de visualisation de données forte valeur ajoutée. Le premier service MarsSI a pour objectif est de combiner les données multi-sources de quatre missions orbitales documentant la surface de Mars (données de topographie, minéralogie et imagerie). Ce service permet via une interface géographique de sélectionner, télécharger depuis les serveurs NASA ou ESA et traiter tout type de données de la surface de Mars. Le second service produit, archive et distribue les données valeurs ajoutées issues de missions spatiales et en mettant en avant plus particulièrement les jeux de donnés sous la responsabilité des OSU impliqués. Ces produits sont des cartes globales et locales des propriétés de la surface (composition chimique et minéralogique, propriétés physiques), des cartographies géomorphologies vectorielles, ainsi que les produits MarsSI tels que décrits précédemment. Consultation BDD

Centre Jean-Marie Mariotti

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OSUG Michel DIETRICH Gilles DUVERT [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OCA Thierry LANZ Alexis MATTER [email protected] OSUL Isabelle DANIEL Obs. Paris Claude CATALA

Description

Le Centre Jean-Marie Mariotti est le Pôle National de Données d'interférométrie Optique et Infrarouge. Il coordonne les activités de deux Services Nationaux d'Observation:

- le SNO5 Méthodes et Outils pour l'Interférométrie Optique (MOIO) - le SNO3 Service aux Utilisateurs du VLTI (SUV)

Ce service ne possède pas de moyens propres autres que sa Direction. Il est doté d'un Conseil Scientifique de 12 membres indépendants et d'un Comité de Direction constitué du Directeur Adjoint Scientifique de l'INSU-AA (président), des directions des 4 établissements partenaires représentés par les directeurs d'OSU de ces établissements, du président de l'ASHRA. La Direction du JMMC assiste aux Comité de direction en tant que membre invité.

Une convention (en cours de renouvellement) précise les modalités de l'action du JMMC et de ses comités: http://www.mariotti.fr/doc/approved/JMMC-GEN-0000-0006.pdf Consultation BDD

Pôle de diffusion de données de physique atomique et moléculaire

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

Obs. Paris Claude CATALA Franck DELAHAYE [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OASU Marie Lise DUBERNET-TUCKEY Valentine WAKELAM [email protected] THETA Philippe ROUSSELOT Vincent BOUDON [email protected] OMP Michael TOPLIS Charlotte VASTEL [email protected] Description

Le pôle thématique diffusion de données de physique atomique et moléculaire a pour mission de:

- Coordonner l'ensemble des activités nationales de diffusion des données atomiques et moléculaires. - Diffuser et promouvoir les services de diffusion de données de physique atomique et moléculaire en France. - Favoriser la mutualisation et le partage des compétences et savoirs pour permettre un développement concerté des services généraux et spécifiques. - Evaluer les moyens humains et matériels nécessaires au bon fonctionnement des services labellisés et permettant de répondre aux demandes des utilisateurs (développement de nouveaux services – cf point 3 ci-dessus) et donner un avis consultatif sur les activités françaises vis--vis des instances. - Encourager et soutenir(1) les nouvelles initiatives (services fonctionnels non encore labellisés, nouveaux services largement/massivement sollicités par les utilisateurs via les programmes nationaux ou autres). (1)Le soutien peut se concevoir sous différentes formes (partage de connaissance, conseils pour faciliter l'intégration dans des interfaces/cadres déjexistants, aide la demande de labellisation

L'ensemble des services référencés auprès du pôle au 26 Novembre 2014 est: Les services labellisés: BASECOL - http://basecol.obspm.fr/ CASSIS -http://cassis.irap.omp.eu/ KIDA - http://kida.obs.u-bordeaux1.fr/ Portail VAMDC et services associés - http://portal.vamdc.eu/vamdc_portal/query.seam et http://www.vamdc.eu

Les services non labellisés: ECaSDa - http://vamdc.univ-reims.fr/PHP/ethylene.php – connecté VAMDC MeCaSDa - http://vamdc.icb.cnrs.fr/PHP/methane.php – connecté VAMDC TFMecaSDa - http://vamdc.icb.cnrs.fr/PHP/tfmecasda.php – connecté VAMDC SHeCaSDa - http://vamdc.icb.cnrs.fr/PHP/shecasda.php – connecté VAMDC SESAM - http://sesam.obspm.fr/ – connecté VAMDC STARK-B - http://stark-b.obspm.fr/ – connecté VAMDC TIPBASE - http://cdsweb.u-strasbg.fr/tipbase/home.html – connecté VAMDC TOPBASE - http://cdsweb.u-strasbg.fr/topbase/topbase.html – connecté VAMDC OP opacity tables - http://opacity-cs.obspm.fr/opacity/index.html

Le pôle thématique s'appuie sur son Comité de Pilotage (CoPil) pour mener bien ses missions. Ce CoPil regroupe les différents acteurs principaux de cette thématique (services labellisé ou non), les représentants des centres d'expertise GSO et PDC ainsi qu'un représentant pour chacun des programmes nationaux suivants PCMI, PNP, PNPS. Le pôle organise ainsi les échanges entre les différents producteurs de services entre eux et avec les utilisateurs afin de coordonner et optimiser le maintien et le développement des services existants. Il peut le cas échéant coordonner le développement des nouveaux services. Consultation BDD

KIDA

Type

AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OASU Marie Lise DUBERNET-TUCKEY Valentine WAKELAM [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU

Description

KIDA pour KInetic Database for Astrochemistry (http://kida.obs.u-bordeaux1.fr/) est une base de données de cinétique chimique (de la phase gazeuse et hétérogène la surface des grains) d'intérêt astrophysique (milieu interstellaire et atmosphères planétaires) avec valeur ajoutée. En effet, un groupe d'experts autour de KIDA propose des recommandations sur des gammes de températures définies. KIDA est régulièrement complétée et mise jour au fur et mesure de nouvelles mesures ou calculs. La base est internationale et plus d'une vingtaine d'astrochimistes participent son amélioration. Ce service est inclus dans le pôle de diffusion des données de physique atomique et moléculaire ainsi que dans le centre d’expertise Grand Sud Ouest. Un des grands atouts de KIDA est de permettre la centralisation du travail d’amélioration des données notamment au niveau Français, où il y a une grande communauté de physico-chimistes. En parallèle de KIDA, nous avons créé une base de données d'abondances observées (InterStellar Abundances - ISA, http://isa.obs.u-bordeaux1.fr/) qui regroupe les abondances publiées dans la littérature pour les objets typiques tels que les nuages denses, les enveloppes protostellaires, les régions diffuses, les régions de photo-dissociations. Il n'y a pas de réflexion critique autour des données et toutes les données publiées peuvent y apparaître. Les espèces listées dans ISA sont les mêmes que celles de KIDA et les valeurs contenues dans cette base sont affichées dans les données spécifiques aux molécules dans KIDA. Afin d'améliorer la diffusion des résultats d'astrochimie, en lien avec KIDA ou non, nous avons également créé une liste de diffusion des articles récents dans le domaine: Astrochemical Newsletter (ACN). La soumission des articles se fait par le biais d'un formulaire en ligne (http://acn.obs.u-bordeaux1.fr/) ainsi que l'inscription la liste. Une newsletter contenant les articles du mois est ensuite envoyé tous les mois par email cette liste. Les articles sont également postés au cours du mois sur un compte Facebook. Il y a plus de 500 abonnés la liste mail et au compte Facebook. Consultation BDD

STORMS

Type

AA-ANO6, AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Alexis Paul ROUILLARD [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU OSUPS Nabila AGHANIM Description

Un ensemble de services dédiés l'étude des Relations Soleil-Terre est développé au sein de l'OMP et a vocation constituer un des services (STORMS) du centre d'expertise GSO Data Centre labellisé par l'INSU. STORMS se rattache aux pôles thématiques CDPP et MEDOC labellisés par l'INSU (page internet: http://ov-gso.irap.omp.eu/doku.php? id=projets:relations_soleil-terre#les_outils). Le développement du pôle Relations Soleil-Terre s'articule autour de quatre axes principaux :

• Outils scientifiques : conception, suivi du développement et maintenance d’outils interdisciplinaires permettant entre autres de relier les bases de données françaises (ex. ‘Propagation Tool’) : observations électromagnétiques du Soleil (MEDOC, BASS2000) et du vent solaire (MEDOC) avec les données plasma mesurées in situ (CDPP).

• Outils météorologiques : conception et suivi du développement d’outils permettant de faire des prévisions météorologiques spatiales. Le pôle utilisera ces outils pour ses activités scientifiques, mais ces outils seront aussi conçus pour être directement utilisables par les centres de météorologie de l’espace / l’armée de l’air dans le cadre d’accords définir.

• Réduction des données pour fournir des produits systématiques et synthétiques : transformation des données brutes (Niveau 0) ou calibrées (Niveau 1) en des formes synthétiques/résumées (Niveau 2,3) utilisées par nos outils scientifiques et météorologiques. Ce processus de transformation de données stockées par les bases de données en France contribue leur valorisation. En effet, les missions spatiales telles que SDO ou STEREO produisent plusieurs téraoctets de données par jour. Il est donc nécessaire de les transformer pour les rendre plus aisément manipulables et pour offrir aux chercheurs une visualisation synthétique de l’ensemble de ces données (tout en gardant les liens directs vers les bases de données distribuant ces données).

• Création, collection et mise en ligne de catalogues : le pôle se charge aussi de créer et de rassembler les catalogues de structures observées dans les données d’imagerie et les mesures in-situ. Ces catalogues (i) seront ensuite intégrés dans nos outils scientifiques afin de mutualiser les efforts et les résultats des travaux de chercheurs dans le monde entier et (ii) seront rendus accessibles via les observatoires virtuels de la discipline.

• Définition des instruments et missions futures dédiées la météorologie de l’espace : le service contribue la conception d’instruments et de missions spatiales dédiés. Ceci comprend par exemple les efforts actuels de conception d’instruments « particules » compacts, susceptibles d’être embarqués moindre ressource sur tous types de plateforme, scientifique ou commerciale (AMBRE/AMBRE_GEO). L’utilisation des outils développés par le pôle permettra également de définir les besoins en termes de missions spatiales futures, de type INSTANT (INvestigation of Solar Terrestrial Associated Natural Threats ; mission d’observation au point de Lagrange L5) soumise dans le cadre de la prospective CNES 2014. L’expertise du pôle permettra ensuite de traiter, de distribuer et de mettre en valeur les données obtenues. Consultation BDD

Centre de données de la Physique des Plasmas (CDPP)

Type

AA-ANO6, AA-ANO5

Coordination

Intitulé OSU Directeur de l'OSU Responsable du SNO Email du responsable du SNO

OMP Michael TOPLIS Vincent GENOT [email protected]

Partenaires

Intitulé OSU Directeur de l'OSU Resp. du SNO dans l'OSU Email du resp. du SNO dans l'OSU Obs. Paris Claude CATALA Baptiste CECCONI [email protected]

Description

The CDPP (Centre de Données de Physique des Plasmas) was created in 1998 jointly by CNES and INSU. Université Paul Sabatier, Toulouse and the Observatoire de Paris are now also official partners. The CDPP is the French national data centre for natural plasmas of the solar system. The CDPP assures the long term preservation of data obtained primarily from instruments built using French resources (Cluster, Rosetta, Solar Orbiter among many other), and renders them readily accessible to and exploitable by the international community. The CDPP also provides services to allow user defined data visualisation, merging, computation, search and extraction on data content (see AMDA, the Automated Multi-Dataset Analysis service). Other tools enable to visualize data and models in 3D planetary context (3DView), to correlate solar perturbations to in-situ data by computing propagation times (Propagation Tool) and to apply vector transformations from one coordinate system to other (TREPS). The CDPP is involved in the development of interoperability, and participates in several Virtual Observatory projects (Europlanet, Helio, Vispanet, IMPEx). Annexe II : Liste des publications 2014- 2018

Publications `acomit´ede lecture: ann´ee2014

• Abou Mrad, N., F. Duvernay, P. Theule, T. Chiavassa and G. Danger. 2014. Development and optimization of an analytical system for the Volatile organic compounds Analysis coming from the Heating of Interstellar/cometary Ice Analogs. Analytical Chemistry, 2014, 86, 8391- 8399.

• Ag´undez,M., Biver, N., Santos-Sanz, P., Bockel´ee-Morvan, D., Moreno, R. 2014. Molecular observations of comets C/2012 S1 (ISON) and C/2013 R1 (Lovejoy): HNC/HCN ratios and

upper limits to PH3. Astronomy and Astrophysics 564, L2.

• Ag´undez,M., Parmentier, V., Venot, O., Hersant, F., Selsis, F. 2014. Pseudo 2D chemical model of hot-Jupiter atmospheres: application to HD 209458b and HD 189733b. Astronomy and Astrophysics 564, A73.

• Ag´undez,M., Venot, O., Selsis, F., Iro, N. 2014. The Puzzling Chemical Composition of GJ 436b’s Atmosphere: Influence of Tidal Heating on the Chemistry. The Astrophysical Journal 781, 68.

• Alata, I., Cruz-Diaz, G. A., Mu˜nozCaro, G. M., Dartois, E. 2014. Vacuum ultraviolet pho-

tolysis of hydrogenated amorphous carbons . I. Interstellar H2 and CH4 formation rates. Astronomy and Astrophysics 569, A119.

• Ali-Dib, M., Mousis, O., Pekmezci, G. S., Lunine, J. I., Madhusudhan, N., Petit, J.-M. 2014. Influence of the C/O ratio on titanium and vanadium oxides in protoplanetary disks. Astronomy and Astrophysics 561, A60.

• Ali-Dib, M., Mousis, O., Petit, J.-M., Lunine, J. I. 2014. Carbon-rich Planet Formation in a Solar Composition Disk. The Astrophysical Journal 785, 125.

• Ali-Dib, M., Mousis, O., Petit, J.-M., Lunine, J. I. 2014. The Measured Compositions of Uranus and Neptune from their Formation on the CO Ice Line. The Astrophysical Journal 793, 9.

• Al´ı-Lagoa,V., Lionni, L., Delbo, M., Gundlach, B., Blum, J., Licandro, J. 2014. Thermo-

physical properties of near-Earth asteroid (341843) 2008 EV5 from WISE data. Astronomy and Astrophysics 561, A45.

• Alonso, R., and 50 colleagues 2014. Transiting exoplanets from the CoRoT space mission. XXVI. CoRoT-24: a transiting multiplanet system. Astronomy and Astrophysics 567, A112.

• Altobelli, N., Lopez-Paz, D., Pilorz, S., Spilker, L. J., Morishima, R., Brooks, S., Leyrat, C., Deau, E., Edgington, S., Flandes, A. 2014. Two numerical models designed to reproduce Saturn ring temperatures as measured by Cassini-CIRS. Icarus 238, 205-220. • Alvarez-Candal, A., and 11 colleagues 2014. Stellar occultation by (119951) 2002 KX14 on April 26, 2012. Astronomy and Astrophysics 571, A48. Amiguet, E., B. V

• an De Moortle, P. Cordier, N. Hilairet, B. Reynard, Deformation mechanisms and rheology of serpentines in experiments and in nature, Journal of Geophysical Research 119 (2014)

• Amiguet, E., Van De Moortle B., Cordier P., Hilairet N., Reynard B. (2014) Deformation mechanisms and rheology of serpentines in experiments and in nature, Journal of Geophysical Research-Solid Earth.

• Amit, H. 2014. Can downwelling at the top of the Earth’s core be detected in the geomagnetic secular variation?. Physics of the Earth and Planetary Interiors 229, 110-121.

• Amodeo, J., B. Devincre, P. Carrez, P. Cordier, Dislocation reactions, plastic anisotropy and forest strengthening in MgO at high temperature, Mechanics of Materials 71 pp. 62-73 (2014)

• Amundsen, D. S., Baraffe, I., Tremblin, P., Manners, J., Hayek, W., Mayne, N. J., Acreman, D. M. 2014. Accuracy tests of radiation schemes used in hot Jupiter global circulation models. Astronomy and Astrophysics 564, A59.

• Aresu, G., and 10 colleagues 2014. [O I] disk emission in the Taurus star-forming region. Astronomy and Astrophysics 566, A14.

• Arlot, J.-E., and 93 colleagues 2014. The PHEMU09 catalogue and astrometric results of the observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made in 2009. Astronomy and Astrophysics 572, A120.

• Arnold, L., and 11 colleagues 2014. The Earth as an extrasolar transiting planet. II. HARPS

and UVES detection of water vapour, biogenic O2, and O3. Astronomy and Astrophysics 564, A58.

• Arridge, C. S., and 113 colleagues 2014. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets. Planetary and Space Science 104, 122-140.

• Arvidson, R. E., and 27 colleagues 2014. Terrain physical properties derived from orbital data and the first 360 sols of Mars Science Laboratory Curiosity rover observations in Gale Crater. Journal of Geophysical Research (Planets) 119, 1322-1344.

• Astafyeva, E., Rolland, L. M., Sladen, A. 2014. Strike-slip earthquakes can also be detected in the ionosphere. Earth and Planetary Science Letters 405, 180-193.

• Ataiee, S., Dullemond, C. P., Kley, W., Reg´aly, Z., Meheut, H. 2014. Planet-vortex inter- action: How a vortex can shepherd a planetary embryo. Astronomy and Astrophysics 572, A61. • Aubert, J. 2014. Earth’s core internal dynamics 1840-2010 imaged by inverse geodynamo modelling. Geophysical Journal International 197, 1321-1334.

• Aubert, J. 2014. Erratum to: Earth’s core internal dynamics 1840-2010 imaged by inverse geodynamo modelling. Geophysical Journal International 198, 1683-1683.

• Auclair-Desrotour, P., Le Poncin-Lafitte, C., Mathis, S. 2014. Impact of the frequency de- pendence of tidal Q on the evolution of planetary systems. Astronomy and Astrophysics 561, L7.

• Audouard, J., Poulet, F., Vincendon, M., Bibring, J.-P., Forget, F., Langevin, Y., Gondet, B. 2014. Mars surface thermal inertia and heterogeneities from OMEGA/MEX. Icarus 233, 194-213.

• Audouard, J., Poulet, F., Vincendon, M., Milliken, R. E., Jouglet, D., Bibring, J.-P., Gondet, B., Langevin, Y. 2014. Water in the Martian regolith from OMEGA/Mars Express. Journal of Geophysical Research (Planets) 119, 1969-1989.

• Auriac, A., Sigmundsson, F., Hooper, A., Spaans, K. H., Bj¨ornsson, H., P´alsson,F., Pinel, V., Feigl, K. L. 2014. InSAR observations and models of crustal deformation due to a glacial surge in Iceland. Geophysical Journal International 198, 1329-1341.

• Avice, G., Marty, B. 2014. The iodine-plutonium-xenon age of the Moon-Earth system re- visited. Philosophical Transactions of the Royal Society of London Series A 372, 20130260- 20130260.

• Badro, J. 2014. Spin Transitions in Mantle Minerals. Annual Review of Earth and Planetary Sciences 42, 231-248.

• Bailli´e,K., Charnoz, S. 2014. Time Evolution of a Viscous Protoplanetary Disk with a Free Geometry: Toward a More Self-consistent Picture. The Astrophysical Journal 786, 35.

• Baland, R.-M., Tobie, G., Lef`evre,A., Van Hoolst, T. 2014. Titan’s internal structure inferred from its gravity field, shape, and rotation state. Icarus 237, 29-41.

• Balan, E., M. Blanchard, M. Lazzeri, J. Ingrin, Contribution of interstitial OH groups to the incorporation of water in forsterite, Physics and Chemistry of Minerals 41 pp. 105-114 (2014)

• Ballouz, R.-L., Richardson, D. C., Michel, P., Schwartz, S. R. 2014. Rotation-dependent Catastrophic Disruption of Gravitational Aggregates. The Astrophysical Journal 789, 158.

• Baraffe, I., Chabrier, G., Fortney, J., Sotin, C. 2014. Planetary Internal Structures. Protostars and Planets VI 763-786.

• Baratoux, D., Samuel, H., Michaut, C., Toplis, M. J., Monnereau, M., Wieczorek, M., Garcia, R., Kurita, K. 2014. Petrological constraints on the density of the Martian crust. Journal of Geophysical Research (Planets) 119, 1707-1727. • Baratta, G. A., Chaput, D., Cottin, H., Fernandez Cascales, L., Palumbo, M. E., Strazzulla, G. 2015. Organic samples produced by ion bombardment of ices for the EXPOSE-R2 mission on the International Space Station. Planetary and Space Science 118, 211-220.

• Barnes, J. W., Sotin, C., Soderblom, J. M., Brown, R. H., Hayes, A. G., Donelan, M., Rodriguez, S., Le Mouelic, S., Baines, K. H., McCord, T. B. 2014. Cassini/VIMS Observes Rough Surfaces on Titan’s Punga Mare in Specular Reflection. Planetary Science 3, 3.

• Barrat, J. A., Jambon, A., Ferri`ere,L., Bollinger, C., Langlade, J. A., Liorzou, C., Boudouma, O., Fialin, M. 2014. No Martian soil component in shergottite meteorites. Geochimica et Cosmochimica Acta 125, 23-33.

• Barrat, J.-A., Yamaguchi, A. 2014. Comment on “The origin of eucrites, diogenites, and olivine diogenites: Magma ocean crystallization and shallow magma processes on Vesta” by B. E. Mandler and L. T. Elkins-Tanton. Meteoritics and Planetary Science 49, 468-472.

• Barrat, J. A., Zanda, B., Jambon, A., Bollinger, C. 2014. The lithophile trace elements in enstatite chondrites. Geochimica et Cosmochimica Acta 128, 71-94.

• Barros, S. C. C., and 11 colleagues 2014. SOPHIE velocimetry of Kepler transit candidates. X. KOI-142 c: first radial velocity confirmation of a non-transiting exoplanet discovered by transit timing. Astronomy and Astrophysics 561, L1.

• Barros, S. C. C., and 31 colleagues 2014. Revisiting the transits of CoRoT-7b at a lower activity level. Astronomy and Astrophysics 569, A74.

• Barry, P. H., Hilton, D. R., F¨uri,E., Halld´orsson,S. A., Gr¨onvold, K. 2014. Carbon isotope and abundance systematics of Icelandic geothermal gases, fluids and subglacial basalts with

implications for mantle plume-related CO2 fluxes. Geochimica et Cosmochimica Acta 134, 74-99.

• Barth´elemy, M., Lamy, L., Menager, H., Schulik, M., Bernard, D., Abgrall, H., Roueff, E.,

Cessateur, G., Prange, R., Lilensten, J. 2014. Dayglow and auroral emissions of Uranus in H2 FUV bands. Icarus 239, 160-167.

• Bartoli, O., Cesare, B., Remusat, L., Acosta-Vigil, A., Poli, S. 2014. The H2O content of granite embryos. Earth and Planetary Science Letters 395, 281-290.

• Baruteau, C., Crida, A., Paardekooper, S.-J., Masset, F., Guilet, J., Bitsch, B., Nelson, R., Kley, W., Papaloizou, J. 2014. Planet-Disk Interactions and Early Evolution of Planetary Systems. Protostars and Planets VI 667-689.

• Batista, V., Beaulieu, J.-P., Gould, A., Bennett, D. P., Yee, J. C., Fukui, A., Gaudi, B. S., Sumi, T., Udalski, A. 2014. MOA-2011-BLG-293Lb: First Microlensing Planet Possibly in the Habitable Zone. The Astrophysical Journal 780, 54. • Beam´ın,J. C., and 12 colleagues 2014. Temperature constraints on the coldest brown dwarf known: WISE 0855-0714. Astronomy and Astrophysics 570, L8.

• Bechtel, H. A., and 67 colleagues 2014. Stardust Interstellar Preliminary Examination III: In- frared spectroscopic analysis of interstellar dust candidates. Meteoritics and Planetary Science 49, 1548-1561.

• Beck, P., Garenne, A., Quirico, E., Bonal, L., Montes-Hernandez, G., Moynier, F., Schmitt, B. 2014. Transmission infrared spectra (2-25 µm) of carbonaceous chondrites (CI, CM, CV-CK, CR, C2 ungrouped): Mineralogy, water, and asteroidal processes. Icarus 229, 263-277.

• Beck, P., Quirico, E., Garenne, A., Yin, Q.-Z., Bonal, L., Schmitt, B., Montes-Hernandez, G., Montagnac, G., Chiriac, R., Toche, F. 2014. The secondary history of Sutter’s Mill CM carbonaceous chondrite based on water abundance and the structure of its organic matter from two clasts. Meteoritics and Planetary Science 49, 2064-2073.

• Beichman, C., and 47 colleagues 2014. Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST). Publications of the Astronomical Society of the Pacific 126, 1134.

• Belissont, R., Boiron, M.-C., Luais, B., Cathelineau, M. 2014. LA-ICP-MS analyses of minor and trace elements and bulk Ge isotopes in zoned Ge-rich sphalerites from the Noailhac - Saint-Salvy deposit (France): Insights into incorporation mechanisms and ore deposition processes. Geochimica et Cosmochimica Acta 126, 518-540.

• Bellili A., Schwell M., Benilan Y., Fray N., Gazeau M.-C., Mogren Al-Mogren M., Guillemin J.-C., Poisson L. and H. Hochlaf (2014) VUV photoionization and dissociative photoionization of the prebiotic molecule acetyl cyanide : Theory and experiment. Journal of Chemical Physics, 141(13), 134311.

• Bello L., N. Coltice, T. Rolf, P.J. Tackley, On the predictability limit of convection models of the Earth’s mantle, Geochemistry, Geophysics, Geosystems, Volume 15, Issue 6, pp. 2319- 2328, 2014.

• Benecchi, S. D., and 10 colleagues 2014. The UT 7/8 February 2013 Sila-Nunam mutual event & future predictions. Icarus 229, 423-427.

• Ben-Jaffel, L., Ballester, G. E. 2014. Transit of Exomoon Plasma Tori: New Diagnosis. The Astrophysical Journal 785, L30.

• Bennett, D. P., and 99 colleagues 2014. MOA-2011-BLG-262Lb: A Sub-Earth-Mass Moon Orbiting a Gas Giant Primary or a High Velocity Planetary System in the Galactic Bulge. The Astrophysical Journal 785, 155. • Berger, G., Meunier, A., Beaufort, D. 2014. Clay mineral formation on Mars: Chemical constraints and possible contribution of basalt out-gassing. Planetary and Space Science 95, 25-32.

• Bernard, D., Lilensten, J., Barth´elemy, M., Gronoff, G. 2014. Can hydrogen coronae be

inferred around a CO2-dominated exoplanetary atmosphere?. Icarus 239, 23-31.

• Bertaux, J.-L., Combi, M. R., Qu´emerais,E., Schmidt, W. 2014. The water production rate of Rosetta target Comet 67P/Churyumov-Gerasimenko near perihelion in 1996, 2002 and 2009 from Lyman α observations with SWAN/SOHO. Planetary and Space Science 91, 14-19.

• Bertaux, J. L., Lallement, R., Ferron, S., Boonne, C., Bodichon, R. 2014. TAPAS, a web-based service of atmospheric transmission computation for astronomy. Astronomy and Astrophysics 564, A46.

• Berthier, J., Vachier, F., Marchis, F., Durech,ˇ J., Carry, B. 2014. Physical and dynamical properties of the main belt triple Asteroid (87) Sylvia. Icarus 239, 118-130.

• Bertrand, M., Chabin, A., Colas, C., Cad`ene,M., Chaput, D., Brack, A., Cottin, H. 2015. The AMINO experiment: exposure of amino acids in the EXPOSE-R experiment on the International Space Station and in laboratory. International Journal of Astrobiology 14, 89- 97.

• Besserer, J., Nimmo, F., Wieczorek, M. A., Weber, R. C., Kiefer, W. S., McGovern, P. J., Andrews-Hanna, J. C., Smith, D. E., Zuber, M. T. 2014. GRAIL gravity constraints on the vertical and lateral density structure of the lunar crust. Geophysical Research Letters 41, 5771-5777.

• Beth, A., Garnier, P., Toublanc, D., Dandouras, I., Mazelle, C., Kotova, A. 2014. Modeling the satellite particle population in the planetary exospheres: Application to Earth, Titan and Mars. Icarus 227, 21-36.

• Beust, H., Augereau, J.-C., Bonsor, A., Graham, J. R., Kalas, P., Lebreton, J., Lagrange, A.- M., Ertel, S., Faramaz, V., Th´ebault, P. 2014. An independent determination of Fomalhaut b’s orbit and the dynamical effects on the outer dust belt. Astronomy and Astrophysics 561, A43.

• Bezacier L., Baptiste JOURNAUX, Jean-Philippe PERRILLAT, Herv CARDON, Michael HANFLAND, Isabelle DANIEL (2014) Equations of state of ice VI and ice VII at high pressure and high temperature, J. Chem. Phys., 141, 104505.

• Bezacier, L., Le Menn, E., Grasset, O., Bollengier, O., Oancea, A., Mezouar, M., Tobie, G. 2014. Experimental investigation of methane hydrates dissociation up to 5 GPa: Implications for Titan’s interior. Physics of the Earth and Planetary Interiors 229, 144-152. • Bezaeva, N. S., and 10 colleagues 2014. Magnetic properties of the LL5 ordinary chondrite Chelyabinsk (fall of February 15, 2013). Meteoritics and Planetary Science 49, 958-977.

• B´ezard,B. 2014. The methane mole fraction in Titan’s stratosphere from DISR measurements during the Huygens probe’s descent. Icarus 242, 64-73.

• Bianchini, G., Bryce, J.G., Blichert-Toft, J., Beccaluva, L., and Natali, C., 2014. Mantle dynamics and secular variations beneath the East African Rift: Insights from peridotite xenoliths (Mega, Ethiopia). Chem. Geol. 386, 49-58.

• Biennier, L., Carles, S., Cordier, D., Guillemin, J.-C., Le Picard, S. D., Faure, A. 2014. Low − temperature reaction kinetics of CN + HC3N and implications for the growth of anions in Titan’s atmosphere. Icarus 227, 123-131.

• Bieryla, A., and 20 colleagues 2014. HAT-P-49b: A 1.7 M J Planet Transiting a Bright 1.5 M sun; F-star. The Astronomical Journal 147, 84.

• Biller, B. A., and 15 colleagues 2014. An Enigmatic Point-like Feature within the HD 169142 Transitional Disk. The Astrophysical Journal 792, L22.

• Birlan, M., Alin Nedelcu, D., Popescu, M., Badescu, O. 2014. Near-Earth Asteroids: Obser- vations Via Remote Observing Techniques. Romanian Astronomical Journal 24, 119.

• Birlan, M., Nedelcu, D. A., Popescu, M., Vernazza, P., Colas, F., Kryszczy´nska, A. 2014. Spectroscopy and surface properties of (809) Lundia. Monthly Notices of the Royal Astro- nomical Society 437, 176-184.

• Bitsch, B., Morbidelli, A., Lega, E., Crida, A. 2014. Stellar irradiated discs and implications on migration of embedded planets. II. Accreting-discs. Astronomy and Astrophysics 564, A135.

• Bitsch, B., Morbidelli, A., Lega, E., Kretke, K., Crida, A. 2014. Stellar irradiated discs and implications on migration of embedded planets. III. Viscosity transitions. Astronomy and Astrophysics 570, A75.

• Biver, N., and 11 colleagues 2014. Complex organic molecules in comets C/2012 F6 (Lem- mon) and C/2013 R1 (Lovejoy): detection of ethylene glycol and formamide. Astronomy and Astrophysics 566, L5.

• Blaney, D. L., and 31 colleagues 2014. Chemistry and texture of the rocks at Rocknest, Gale Crater: Evidence for sedimentary origin and diagenetic alteration. Journal of Geophysical Research (Planets) 119, 2109-2131.

• Bockel´ee-Morvan, D., and 22 colleagues 2014. Searches for HCl and HF in comets 103P/Hartley 2 and C/2009 P1 (Garradd) with the Herschel Space Observatory. Astronomy and Astro- physics 562, A5. • Bodin, T., Yuan, H., Romanowicz, B. 2014. Inversion of receiver functions without deconvo- lution – application to the Indian craton. Geophysical Journal International 196, 1025-1033.

• Boissel, Y., and 22 colleagues 2014. An exploration of Pluto’s environment through stellar occultations. Astronomy and Astrophysics 561, A144.

• Boissier, J., Bockel´ee-Morvan, D., Biver, N., Colom, P., Crovisier, J., Moreno, R., Zakharov, V., Groussin, O., Jorda, L., Lis, D. C. 2014. Gas and dust productions of Comet 103P/Hartley 2 from millimetre observations: Interpreting rotation-induced time variations. Icarus 228, 197- 216.

• Bollinger, C., P. Raterron, P. Cordier, S. Merkel, Polycrystalline olivine rheology in dislocation creep: Revisiting experimental data to 8.1GPa, Physics of the Earth and Planetary Interiors 228 pp. 211-219 (2014)

• Bolmont, E., Raymond, S. N., von Paris, P., Selsis, F., Hersant, F., Quintana, E. V., Bar- clay, T. 2014. Formation, Tidal Evolution, and Habitability of the Kepler-186 System. The Astrophysical Journal 793, 3.

• Bonnefoy, M., and 15 colleagues 2014. Physical and orbital properties of β Pictoris b. Astron- omy and Astrophysics 567, L9.

• Bonnefoy, M., and 69 colleagues 2014. Characterization of the gaseous companion κ An- dromedae b. New Keck and LBTI high-contrast observations. Astronomy and Astrophysics 562, A111.

• Bonnet, J.-Y., and 14 colleagues 2015. Formation of analogs of cometary nitrogen-rich refrac- tory organics from thermal degradation of tholin and HCN polymer. Icarus 250, 53-63.

• Bonnin, M., Nolet, G., Villase˜nor,A., Gallart, J., Thomas, C. 2014. Multiple-frequency tomography of the upper mantle beneath the African/Iberian collision zone. Geophysical Journal International 198, 1458-1473.

• Bonsor, A., Raymond, S. N., Augereau, J.-C., Ormel, C. W. 2014. Planetesimal-driven mi- gration as an explanation for observations of high levels of warm, exozodiacal dust. Monthly Notices of the Royal Astronomical Society 441, 2380-2391.

• Borgniet, S., and 21 colleagues 2014. Extrasolar planets and brown dwarfs around A-F type stars. VIII. A giant planet orbiting the young star HD 113337. Astronomy and Astrophysics 561, A65.

• Bouchet, R. A., Blichert-Toft, J., Reid, M. R., Levander, A., Albar`ede,F. 2014. Similarities between the Th/U map of the western US crystalline basement and the seismic properties of the underlying lithosphere. Earth and Planetary Science Letters 391, 243-254. • Boudjada, M. Y., Galopeau, P. H. M., Sawas, S., Lammer, H. 2014. Remote sensing of the Io torus plasma ribbon using natural radio occultation of the Jovian radio emissions. Annales Geophysicae 32, 1119-1128.

• Bou´e,G., Fabrycky, D. C. 2014. Compact Planetary Systems Perturbed by an Inclined Com- panion. II. Stellar Spin-Orbit Evolution. The Astrophysical Journal 789, 111.

• Bou´e,G., Fabrycky, D. C. 2014. Compact Planetary Systems Perturbed by an Inclined Com- panion. I. Vectorial Representation of the Secular Model. The Astrophysical Journal 789, 110.

• Bouilloud, M., Fray, N., B´enilan,Y., Cottin, H., Gazeau, M.-C., Jolly, A. 2015. Bibliographic review and new measurements of the infrared band strengths of pure molecules at 25 K:

H2O, CO2, CO, CH4, NH3, CH3OH, HCOOH and H2CO. Monthly Notices of the Royal Astronomical Society 451, 2145-2160.

• Boujibar, A., Andrault, D., Bouhifd, M. A., Bolfan-Casanova, N., Devidal, J.-L., Trcera, N. 2014. Metal-silicate partitioning of sulphur, new experimental and thermodynamic constraints on planetary accretion. Earth and Planetary Science Letters 391, 42-54.

• Bouley, S., Craddock, R. A. 2014. Age dates of valley network drainage basins and subbasins within Sabae and Arabia Terrae, Mars. Journal of Geophysical Research (Planets) 119, 1302- 1310.

• Bouquet, A., Baratoux, D., Vaubaillon, J., Gritsevich, M. I., Mimoun, D., Mousis, O., Bouley, S. 2014. Simulation of the capabilities of an orbiter for monitoring the entry of interplanetary matter into the terrestrial atmosphere. Planetary and Space Science 103, 238-249.

• Bourrier, V., H´ebrard,G. 2014. Detecting the spin-orbit misalignment of the super-Earth 55 Cancri e. Astronomy and Astrophysics 569, A65.

• Bourrier, V., Lecavelier des Etangs, A., Vidal-Madjar, A. 2014. Modeling magnesium escape from HD 209458b atmosphere. Astronomy and Astrophysics 565, A105.

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ANNÉE 2015 Porteur du projet Titre du projet theme Financement en Keu Modélisation et Simulation des Disques de Débris et AUGEREAU Jean-Charles 1 5 Exozodiacaux Mesure de masses des exoplanètes découvertes par BEAULIEU Jean-Philippe 1 6 microlensing. BOUCHY Francois Colloque OHP-2015 : twenty years of giant exoplanets 1 2 Recherche et caractérisation des planètes par BOUCHY Francois 1 3 vélocimétrie radiale CHAUVIN Gael Action Coordonée Exploitation SPHERE 1 9 Recherche et caractérisation de planètes autour d'étoiles DELFOSSE Xavier 1 5 de très faible masse Di FOLCO EmMANUEL Disques de transition et disques de débris 1 2 Modélisation de l'opacité des planètes extra solaires de GEORGES Robert 1 3 type Jupiter chaud et Neptune chaud GONZALEZ Jean-François Régions internes des disques protoplanétaires 1 2,5 Participation au colloque international 2015 de l'IAP : HEBRARD Guillaume 1 2 "From super-Earths to brown dwarfs: Who's Who?" LESTRADE Jean-Francois Etudes des disques de débris avec HERSCHEL 1 5 Marées et interactions MHD dans les systèmes MATHIS Stéphane 2b/1 6 planétaires SALOME Philippe IYAS 2015 1/2b/4 1 Atmosphères et climats des exoplanètes: simulation et SELSIS Franck 1 2,5 observation BOULEY Sylvain Impact 3D 2b 2

CROVISIER Jacques Observation et modélisation des atmosphères cométaires 2b 6 Identification de familles d?astéroïdes âgées de plus de 2 DELBO Marco 2b 5 Ga DELSANTI Audrey OSSOS - Outer Solar System Origin Survey 2b 2,5 ERARD Stéphane VESPA: Observatoire Virtuel pour le Système solaire 2b 2 Simulations numériques des écoulements de libration et FAVIER Benjamin 3 5 de marées dans les intérieurs planétaires Propriétés physiques et interactions des petits corps du FORNASIER Sonia système solaire par l'observation à partir du sol et de 2b 8 l'espace OREGOC (ORigine et Evolution des Glaces et des FRAY Nicolas 2b 3 Composés Organiques Cométaires) RAMBAUX Nicolas Rotation des corps célestes 2b 4 Un nouveau champ d?impactites dans le désert d?Atacama, Chili. Implications pour la compréhension des ROPERCH Pierrick 2b 6 effets au sol lors de la désintégration d?un astéroïde dans l?atmosphère. Apport de contraintes sur les modèles de formation du ROUSSELOT Philippe système solaire externe à partir d'observations et de 2b 8 modélisation SCHMIDER François- JIVE (Jovian Interiors from Velocimetry Experiment) 2b 7,5 Xavier Gaia-FUN-NEO: Etude d'objets géocroiseurs détectés par THUILLOT William 2b 2 Gaia Spectrophotométrie des météorites primitives: BECK Pierre 2a/2b 7 reconstruire le lien avec les petits corps. Age de la première croûte lunaire ? Etude du système BOYET Maud 2a 6 146Sm-142Nd Sur la différence de composition isotopique en oxygène CARTIGNY Pierre 2a 7 entre Terre, Lune et Chondrites à Enstatite A la recherche de la radioactivité éteinte du 32Si dans le CHAUSSIDON Marc 2a 8 disque d'accrétion Synthèse de matière organique analogue à celle des DERENNE Sylvie 2a 7,5 météorites carbonées DEVOUARD Bertrand A new tektite strewnfield in Atacama, Chile 2a 3 Photoionisation du radical CN : mesure précise du seuil DOUIN Stéphane d?ionisation et de la section efficace pour la 2a 4 mode?lisation de la chimie de l?azote Origine et signification des inclusions vitreuses riches en FAURE François 2a 2,5 silice dans les olivines des chondres de type I. Coupled H- and N-noble gas analyses of lunar basalts: FURI Evelyn Constraints on the origin and evolution of volatiles in the 2a 10 Earth-Moon system Les chromites dans les chondrites: marqueurs GOPEL Christa isotopiques pour les radioactivités éteintes Cr/Mn, et 2a 7 Al/Mg et pour les isotopes d?oxygène Evolution de la composition isotopique de l'oxygene des GOUNELLE Matthieu 2a 8 carbonates dans les astéroïdes hydratés L?étude CRESU de la chimie de l?azote atomique à basse HICKSON Kevin 2a 5 température LUAIS Béatrice Origine des pallasites : apport des éléments sidérophiles 2a 5 Irradiation dans le système solaire en formation: MOREIRA Manuel implications pour l'incorporation des gaz rares dans les 2a/3 5 chondrites et la Terre ALBOUSSIERE Thierry Expériences de convection compressible (EXCC) 3 5 Constraints on telluric planetary cores by sound velocity ANTONANGELI Daniele 3 5 and density measurements Imagerie sismique de la lithosphère cratonique par BONDIN Thomas 3 5 méthodes trans-dimensionelles Effets du Carbone et de l'Hydrogène sur la ségrégation BOUHIFD Mohamed Ali noyau-manteau des planètes telluriques: cas de la Terre 3/5/ 7 et Mars Crystallographic preferred orientations of enstatite BYSTRICKY Micha 3 3 deformed at upper mantle pressures and temperatures Interprétation texturale de la structure sismologique de la CALVET marie 3 4 graine : observations et modélisation Terres cuites archéologiques et spéléothèmes : deux CAMPS PIERRE archives complémentaires des fluctuations du Champ 3 3,5 Magnétique Terrestre au cours de l?Holocène. Brassage des hétérogénéités dans les panaches : FARNETANI Cinzia 3 5 expériences de laboratoire et simulations numériques Fluctuations extrêmes du champ archéomagnétique et FOURNIER Alexandre 3 3 dynamique du noyau Détermination de la solubilité de H2O & CO2 dans les FRANCE Lyderic magmas phonolitiques : application à la caractérisation 3 2,5 de la plomberie de l?Oldoinyo Lengai (Tanzanie) Etude Expérimentale de la Plasticité des Manteaux HILAIRET Nadege 3 6,5 Planétaires H-Olivine project : Une approche expérimentale et INGRIN Jannick 3 6,5 numérique couplée Multi-stage formation, evolution and delamination of IONOV Dmitri lithospheric mantle in the Siberian craton: insights from 3 8,5 xenoliths in Obnazhennaya kimberlite Convection dans le manteau en interaction avec un océan LABROSSE Stéphane 3/ 3,5 de magma Caractériser les hétérogénéités de la lune : approche de MARGERIN Ludovic 3 5 transfert radiatif Inversion conjointe multi-échelle de formes d?onde MARTIN Roland télésismiques et d'anomalies gravimétriques par 3 6,5 éléments spectraux Atténuation sismique de l?olivine : mesures PERRILLAT Jean-Philippe expérimentales aux conditions du manteau supérieur et 3 4,5 fréquences sismiques Variation séculaire du champ magnétique terrestre à PERRIN Mireille 3 7 l'Holocène Composition du noyau rocheux des grands satellites et REYNARD Bruno 3/2b 4 astéroïdes Apport de la gravimétrie terrestre à la détermination du ROGISTER Yves 3 3 mouvement du géocentre Le Champ magnétique terrestre au crépuscule du ROUSSE Sonia Précambrien : basculement de la terre ou variations de 3 7,5 géométrie ? GOCE, GRACE, CHAMP, et Swarm, des opportunités pour THEBAULT Erwan 3 4,5 imager globalement la lithosphère terrestre. Inversion conjointe des données sismologiques Apollo et WIECZOREK Mark 3 3 gravimétriques GRAIL Les atmosphères des planètes géantes: observations avec BILLEBAUD Françoise 4 6 Herschel et ALMA et modélisation photochimique Modélisation de la sublimation comme agent CARPY Sabrina 4 7 géomorphologique à la surface des planètes CHAUFRAY Jean-Yves Modélisation 3D de la haute atmosphère de Mars 4 2

COUTURIER-TAMBURELLI Photochimie des Aérosols de Titan 4 5 Isabelle Interactions climat/morphologie sur Mars : GARGANI Julien caractérisation des activités saisonnières actuelles et des 4 7,5 milieux froids récents LAVVAS Panayotis Atmospheric molecular growth 4 5

LEBLANC Francois Modélisation 3D des exosphères Galiléennes 4 4 LEFEVRE Franck ATMARVEN 4 7,5

LE PICARD SEBASTIEN Photochimie de l'atmosphère de Titan 4 4,5 Colloque international « 3rd Planetary cryosphere MASSE Marion 4 1 workshop » Magmatisme des planètes telluriques, détection, MICHAUT Chloé caractérisation et conséquences sur l?évolution de la 4 4 croûte. Caractérisation spectroscopique des planètes géantes et MORENO Raphael 2b/4 5 de leur système Analyse géomorphologique et modélisation des POCHAT Stéphane processus sous-glaciaires sur Mars (Fin Noachien / Mi- 4 4 Hespérien) Mars, et Pluton : Condensation et métamorphisme de SCHMITT Bernard 4 7,5 leurs neiges (CO2 :H2O, N2 :CH4) Etude de la croissance et de la structure des aérosols de SZOPA Cyril Titan par analyse en 2DGCMS de tholins de Titan produits 4 6 avec l?expérience PAMPRE Etude de l?atmosphère de Titan à partir des données VINATIER Sandrine 4 6 Cassini et ALMA Observations de la dynamique et la composition de WIDEMANN Thomas 4 6 l'atmosphère de Vénus Structure, dynamique et émissions électromagnétiques des magnétosphères de Jupiter, Saturne, et Uranus & ZARKA Philippe 4/1/ 12 Etude des environnements planétaires et recherche d'exoplanètes avec LOFAR, Origin and evolution of silicate reservoirs in the early BLICHERT-TOFT Janne 5 7 Earth Origine de la sidérite dans un lac anoxique et ferrugineux BUSIGNY Vincent 5 6 : implications pour les modèles de Terre primitive Conditions de formation des nodules de pyrites archéens MARIN-CARBONNE ; implications pour la reconstruction des conditions 5 4 Johanna environnementales de la Terre Primitive PHILIPPOT Pascal Le cycle de l?arsenic au Précambrien 5 5 ANNÉE 2016

Porteur du projet Thème Titre du projet

attribution en Euro Atmosphères des planètes extrasolaires et Boccaletti Anthony 1 conditions de formation dans les disques circumstellaires 3000 modélisation de l'opacité des planètes extra GEORGES Robert 1 solaire de type Jupiter chaud et Neptune chaud 4400 Recherche et caractérisation de planètes HEBRARD Guillaume 1 extrasolaires à l?IAP 3000 Keplerian-Stacker : une nouvelle me?thode de Le Coroller Hervé 1 de?tection d?exo-plane?tes et de caracte?risation de leurs parame?tres orbitaux 2500 Etude des disques de débris avec HERSCHEL et Lestrade jean-francois 1 NIKA. 3000 Recherche par maximum d?entropie de jupiters Petit Pascal 1 chauds autour d?étoiles jeunes actives 1300 Atelier National de Spectroscopie Stellaire : Prugniel Philippe 1 Services et outils pour une utilisation optimale des ressources 2000 Modélisation des atmosphères stellaires et ALLARD France 1 planétaires 1000 Modélisation et Simulation des Disques de Débris Augereau Jean-Charles 1 et Exozodiacaux 6000 EARTH-HUNTER : 2016, mesure de masses des Beaulieu Jean-Philippe 1 exoplanètes découvertes par microlensing. 6500

Chauvin Gael 1 Action Nationale Coordonnée SPHERE 10000 Recherche et caractérisation des exoplanètes par BOUCHY Francois 1 vélocimétrie radiale 5000 Recherche et caractérisation de planètes autour Delfosse Xavier 1 d'étoiles de très faible masser 4000

DI FOLCO EMMANUEL 1 Disques de transition et disques de débris 1000 Atmosphères et climats des exoplanètes : Selsis Franck 1 simulation et observation 3000

Chabrier Gilles 1 Equation d'état des intérieurs planétaires 3000 Prédictions théoriques de spectres moléculaires pour les applications astrophysiques à très haute REY Michael 4 température : bases de données pour le méthane, la phosphine et l?éthylène 1000 Volatile abundance and isotope analyses of lunar Füri Evelyn 2a melt inclusions 5500 Composition isotopique du silicium des chondres Villeneuve Johan 2a : Implications sur les interactions solide-gaz dans le disque d?accrétion 5000 Influence des conditions redox sur la HAMMOUDA Tahar 2a condensation des éléments du groupe des terres rares 8000 Réactivité à basse température des radicaux CH Morales Sébastien 2a et C2N en écoulement supersonique uniforme pulsé 6000 Loison Jean-Christophe 2a Chimie du Deutérium 6000 Profils de composition Fe-Mg dans des olivines LEROUX Hugues 2a de la matrice d?Acfer 094 : une origine pré- accrétionnelle ? 4000 Origine et Evolution des Silicates Amorphes des Le Guillou Corentin 2a Matrices de Chondrites Carbonées 10000

Jacquet Emmanuel 2a L'héritage nébulaire des chondres 5000 Atelier « Isomères, Isotopologues et Guillemin jean-Claude 2a Enantiomères. Du Milieu Interstellaire à la Chimie Prébiotique» 1000 Origine et formation des micrométéorites Engrand Cecile 2a cométaires ultracarbonées (UCAMMs) 7000 Processus de déshydratation sous choc de Elmaleh Agnès 2a minéraux analogues des serpentines chondritiques 11000 Etude à l'échelle sub-micrométrique des Aléon-Toppani Alice 2a premiers objets du disque protosolaire 6000 Expériences d'impact à haute vitesse: étude des GANINO Clément 2a fractionnements chimiques et isotopiques associés 7000 Les chromites, témoins de l?histoire et de Gopel Christa 2a l?évolution des corps parents des chondrites ordinaires 4000 Analyses de composés organiques volatils et Danger Gregoire 2a réfractaires provenant de l'altération d'analogues de glaces interstellaire/cométaire 7000 Synthèse d'analogue de matière organique Derenne Sylvie 2a insoluble de météorites 6000

Propriétés spectrales du régolithe d?Itokawa et BONAL Lydie 2b ses relations avec la microstructure subsurface 11100 Quantifier l'hydratation à la surface des BECK Pierre 2b astéroïdes sombres 6000 Évolution de la porosité des grains de poussière Gonzalez Jean-François 2b pendant leur croissance : une solution aux problèmes de formation planétaire ? 1000 Formation des planètes : au-delà des théories Winisdoerffer Christophe 2b linéaires 1500

Vernazza Pierre 2b Formation and evolution of icy small bodies 3000 Soutien au symposium 330 de l'UAI : Recio-Blanco Alejandra 2b "Astrometry and Ast rophysics in the Gaia sky" 1000 Etude théorique et modélisation de la PAUZAT Françoise 2b séquestration des volatils dans les satellites glacés des planètes géantes et les comètes 5200 Organisation d'une conférence internationale en Mathis Stéphane 2b l'honneur de Jean-Paul Zahn 2000

Bouley Sylvain 2b Impact 4D 2000 Etude de sols vitrifiés dans le désert d?Atacama (~13,000 ans BP). Caractérisation des effets ROPERCH Pierrick 2b thermiques au sol lors de la désintégration d?un astéroïde dans l?atmosphère. 7000 Observation et modélisation des atmosphères Crovisier Jacques 2b cométaires 5000

Delbo Marco 2b Primitive asteroids and asteroid families 4500 Propriétés physiques des petits corps du Système Fornasier Sonia 2b Solaire par l'observation à partir du sol et de l'espace 5000 OREGOC - Origine et Evolution des Glaces et des Fray Nicolas 2b composés Organiques Cométaires 3000 Apport de contraintes sur les mode?les de ROUSSELOT Philippe 2b formation du syste?me solaire externe a? partir d?observations et de modélisation 6000 Inversion des paramètres géophysiques à partir Rosat Séverine 3 de la gravimétrie et des nutations 3000 Caractérisation de l?influence du champ de Pinel Virginie 3 contrainte sur le transport de magma grâce aux cratères d?impact. 5000 Quantification de la durée d?un épisode de Moyen Jean-François 3 fusion partielle en contexte de desépaississement tardi-orogénique 5000 Ecoulements de précession dans les intérieurs Meunier Patrice 3 planétaires 5000 Modélisation expérimentale de l'impact d'un deguen renaud 3 planétésimal sur la Terre primitive 7000 Imagerie anisotrope à haute résolution du DEBAYLE Eric 3 continent Américain à partir des données USArray 3500 CHAZOT Gilles 3 ETINDE 6000 Investigation of the Interior Structure, Evolution Mitri Giuseppe 3 and Geological Processes of Icy Bodies in the Outer Solar System 2000 La transformation perovskite/ post-perovskite Merkel Sébastien 3 dans (Mg,Fe)SiO3 : cinétique et effets sur la microsctucture 4000 Constraints on telluric planetary cores by sound Antonangeli Daniele 3 velocity and density measurements 5000

Convection dans les corps planétaires déformés samuel henri 3 par les marées et l?effet de la force de Poincaré 4500

Vers une description de la dynamique rapide Aubert Julien 3 dans les modèles opérationnels de la géodynamo 4500 Outil d'évaluation des méthodes d'analyse de Bonnin Mickaël 3 l'anisotropie sismique; vers une meilleure caractérisation de l'anistropie sismique 3000 Terres cuites archéologiques et spéléothèmes : deux archives complémentaires des fluctuations CAMPS PIERRE 3 du Champ Magnétique Terrestre au cours de l?Holocène. 3500 Realistic geological melts during the giant Caracas Razvan 3 impact: thermodynamics and possible remote identification 5000 Influence de la rhéologie sur la dynamique des Davaille Anne 3 manteaux planétaires: rhéologies anisotropes et rhéologies à mémoire 5500 Crust-mantle coupling and rejuvenation of deep lithosphere in the Siberian craton from data on Dmitri Ionov 3 lower crustal xenoliths and megacrysts in kimberlites 6500 Mantle plumes dynamics: today and back to the farnetani cinzia 3 Archean time 5000 Le champ magnétique terrestre est-il de basse Fournier Alexandre 3 dimensionnalité ? 3000 : Rhéologie des péridotites serpentinisées dans les zones de subduction : approche Hilairet Nadege 3 expérimentale de l?influence de la quantité de déformation 3000 H-Olivine project 2 : Une approche INGRIN Jannick 3 expérimentale et numérique couplée. 6000 Étude analogique de la cristallisation dans un KAMINSKI Edouard 3 océan magmatique 8000 S3MIF2: Impact des espèces radicalaires sur le fractionnement isotopique du soufre Pokrovski Gleb 3 indépendant de la masse (MIF): Applications pour le cycle géochimique du soufre actuel et ancien 6000 Déformation, perméabilité des serpentinites et Reynard Bruno 3 percolation des fluides de subduction 6000 Imagerie de structures complexes dans le Tauzin Benoit 3 manteau par migration de Kirchhoff 5000 Sulfates authigènes formés par sublimation de Rondeau Benjamin 4 glaciers secs : un analogue terrestres pour interpréter les sulfates des autres planètes 7500 Mesures des paramètres collisionnels de H2O REGALIA laurence 4 par CO2. Application à l?étude des atmosphères 2 500 de Vénus et Mars. Conférence internationale « 6th International Massé Marion 4 Conference on Mars Polar Science and 2 000 Exploration » Observations et modélisation des atmosphères MARCQ Emmanuel 4 de Mars et Vénus 7 500 Ionosphère martienne : aurores et dications Lilensten Jean 4 moléculaires 5 000

LAVVAS Panayotis 4 Atmospheric molecular growth 7 000

COSTARD Francois 4 Géomorphologie des processus récents sur Mars 5 500

Hydrocarbures dans la basse atmosphère de Biennier Ludovic 4 Titan : nucléation, condensation et croissance 5 000 des aérosols

Systèmes de minéralisation Ni-Cu-PGE associés Baratoux David 4 au magmatisme Martien 3 000 Modélisation 3D de la haute atmosphère de Chaufray Jean-Yves 4 Mars 2 500 Exploration du système de bandes inconnues du méthane isotopique dans la fenêtre de 2 microns TYUTEREV Vladimir 4 pour l?interprétation des données des missions 6 500 spatiales Etude de l?atmosphère de Titan à partir des Vinatier Sandrine 4 données Cassini et ALMA 7 000 Observations de la dynamique et la composition Widemann Thomas 4 de l'atmosphère de Vénus 3 000 Magnétosphères de Jupiter & Saturne avec Cassini, JUNO et le RDN, et recherche radio ZARKA Philippe 4 d'exoplanètes avec LOFAR, UTR-2 et autres 12 000 instruments au sol

Pochat Stéphane 4 Glaciations Martiennes Anciennes 5 000

Composition et dynamique des planètes géantes Cavalié Thibault 4 et de leur système 6 000 Traçage de l'altération précambrienne par Fabre Sébastien 5 l'isotopie du tungstène 3000 Evolution du systeme du système couplé océan de magma ? atmosphère: apport de la simulation Massol Helene 5 numérique pour contraindre l?histoire précoce des planètes. 5000 Thème Porteur ANNÉE 2017

Thème Nom Titre du projet Attribution

Modélisation des atmosphères stellaires et 1 Allard France planétaires 1000 Modélisation et Simulation des Disques de Débris et 1 Augereau Jean-Charles Exozodiacaux 6000 Tourbillons gaz/poussieres dans les disques 1 Barge Pierre protoplanetaires 3500 EARTH-HUNTER : 2017, mesure de masses des 1 Beaulieu Jean-Philippe exoplanètes découvertes par microlensing. 6000 Atmosphères des planètes extrasolaires et conditions de formation dans les disques 1 Boccaletti Anthony circumstellaires 3000 Recherche et caractérisation de planètes avec le 1 Boisse Isabelle spectrographe SOPHIE 6000 Action Nationale Coordonnée SPHERE 1 Chauvin Gael (consolidation) 5000 Recherche et caractérisation de planètes autour 1 Delfosse Xavier d'étoiles de très faible masse 3000 Chimie des Disques Protoplanétaires: un outil pour 1 dutrey anne comprendre la formation planétaire 1000 1 GUILLOT Tristan Observation de Beta Pic depuis l'Antarctique 3000 Recherche et caractérisation de planètes 1 HEBRARD Guillaume extrasolaires à l'IAP 2250 Etude et modélisation fine d?un nouveau disque de transition détecté sur la tranche par l?instrument SPHERE dans le Upper Centaurus Lupus 1 langlois maud 1500 1 laskar Jacques Dynamical Interactions in Multi-Planet Systems 8000 Keplerian-Stacker : une nouvelle méthode de détection d?exo-planètes et de caractérisation de 1 Le Coroller Hervé leurs paramètres orbitaux 5000 Préparation d?une proposition Early Science Release JWST/MIRI : PAH dans les disques de débris 1 Lestrade jean-francois autour des naines rouges 3000 Bcool : Processus dynamos et cycles magnétiques 1 Morin Julien des étoiles froides 1000 ECOLE EVRY SCHATZMAN 2017 DU PNPS: IMAGERIE A HAUTE RESOLUTION ANGULAIRE DES SURFACES STELLAIRES ET DE LEUR ENVIRONNEMENT PROCHE 1 NARDETTO Nicolas (HRA-étoiles) 2000 Recherche de Jupiters chauds autour d?étoiles 1 Petit Pascal jeunes actives 2000 1 robutel philippe Dynamique et détection de planètes troyennes 3500 Caractérisation de super-Terres et mini-Neptunes 1 Santerne Alexandre en transit avec K2 et HARPS 3500 Statistique de la topographie des planètes et des 1 Schmidt Frédéric exoplanètes 2500 Evolution couplée des systèmes étoile-planète par 1 Strugarek Antoine interactions MHD et marées 7000 Préparation de la mission spatiale JWST : Modélisation Photochimique d?Exoplanètes et 1 VENOT OLIVIA Mesures spectroscopiques à Haute Température 4000 Exoplanètes, interactions plasmas étoile-planète, et 4 ZARKA Philippe émissions radio 5500 Etude à l?échelle sub-micrométrique des premiers 2a Aléon-Toppani Alice objets du disque protosolaire 7000 Signatures radiométriques des structures d?impact en Afrique de l?Ouest, Maghreb, et Australie 2a Baratoux David 6000 CARBOSPIN: Radicaux dans des analogues de 2a Binet Laurent matière carbonée extraterrestre 7000 Analyses en laboratoire de poussières interplanétaires primitives: Préparation à 2a Djouadi-Bouali Zahia l?exploitation des données du JWST. 5000 Les chondres barrés sont-ils symptomatiques d'une 2a Faure François vitesse de refroidissement rapide? 8000 2b GATTACCECA Jérôme Collecte de météorites dans le désert d?Atacama 5000 Atelier « Analyses d'échantillons de la matière 2a Guillemin jean-Claude organique extraterrestre » 1000 Probing the chemical origin of the solar system 2a Janssen Christof oxygen isotopic heterogeneity 3000 Composition moléculaire in situ de la matière organique dans les chondrites: mesures quantitatives en spectroscopie au seuil K du 2a Le guillou Corentin carbone (XANES et EELS). 6000 Caractérisation de l'activité hydrothermale des corps parents des chondrites carbonées de type CV3 2a LIBOUREL Guy 7000 2a moreira manuel L?origine des gaz rares légers sur Terre 7500 Origin of intermediate Z cosmic abundance 2a Simionovici Alexandre depletion 5000 Spectrographe pour Observations en Visible- 2b Birlan Mirel infrarouge d?Astéroïdes Géocroiseurs 3000 Observations et modélisation des atmosphères 2b BIVER Nicolas cométaires 7500 Etude comparative du flux d?impact sur la Lune et 2b Bouley Sylvain Jupiter 4000 2b Commercon Benoit ASTROSIM : école numérique pour l'astrophysique 4000 Contribution au financement d'une école d'hiver : "Chronologie de la Formation du système Solaire VI : le système solaire externe et sa relation avec le 2b CRIDA Aurélien milieu interstellaire" 2500 2b Delbo Marco Primitive asteroids and asteroid families 7000 2b DELSANTI Audrey OSSOS - Outer Solar System Origins Survey 1500 La population des géocroiseurs, traceurs des origines du système solaire et de l?origine de la vie 2b Fornasier Sonia 7500

Des poussières aux planètes : une approche globale 2b Laibe Guillaume 2500 Dynamique des anneaux de Saturne à la lumière des 2b Longaretti Pierre-Yves données Cassini 4000 Apport de contraintes sur les mode?les de formation du syste?me solaire externe a? partir 2b ROUSSELOT Philippe d?observations et de modélisation 9000 Wind tunnel experiments: Calibration for the 2b Vernazza Pierre FRIPON spectroscopic network 5500 3 Alboussiere Thierry PLUIE 5000 Déformation des serpentinites dans les zones de 3 AUZENDE Anne Line subduction 5000 Experimental Study of Earth?s Primordial Magma 3 BADRO James Ocean 8400 3 Barrat Jean-Alix Péridotites d'ici et d'ailleurs 6000 Outils d'évaluation des méthods d'analyse de l'anisotropie sismique; vers une meilleure 3 Bonnin Mickaël caractérisation de l'anisotropie sismique 1000 Quelle source de carbone pour les diamants du 3 Bureau Hélène manteau ? 5000 3 CEBRON David Instabilités inertielles dans les noyaux planétaires 5500 Morphologie des panaches mantelliques et de leur signature en surface en fonction de la rhéologie 3 Davaille Anne complexe du manteau 8400 Etude numérique de l'interaction entre un front de changement de phase et des cellules de convection: océans magmatiques et satellites de glace. 3 Duchemin Laurent 3000 Amplitude et fréquence des variations géomagnétiques extrêmes. Spikes vs pics d?intensité au Moyen-Orient durant le IIIe 3 Gallet Yves millénaire av. J.-C. 6000 Impact dynamique d'une couche stratifiée sur la 3 Gastine Thomas géodynamo 5400 Oscillations centennales à millénaires dans le noyau 3 gillet nicolas terrestre 3500 Non-traditional stable isotopes in the upper mantle and their fractionation in mantle processes 3 Ionov Dmitri 6000 Analyse des données magnétiques satellitaires récentes pour l?identification d?onde dans le noyau 3 lesur vincent liquide de la terre 4500 3 Limare Angela Stability and Evolution of Continental Lithosphere 7400 Apport de la simulation numérique et expérimentale pour contraindre l?histoire précoce des planètes: évolution du système couplé océan de 3 Massol Helene magma ? atmosphère 5500 Transformation perovskite / post-perovskite: 3 Merkel Sébastien mécanismes élémentaires et effet de chimie 7000 Modélisation numérique de l'équilibration thermochimique pendant la ségrégation du fer dans 3 Monteux Julien un océan magmatique. 7000 Migration des magmas carbonatés dans le manteau 3 Perrillat Jean-Philippe terrestre 6400 Caractérisation du champ de contrainte grâce au 3 Pinel Virginie transport de magma sous les cratères d?impact. 3000 Mesures spectroscopiques des seuils de plasticité 3 Reynard Bruno des minéraux du manteau 4000 La forme et la formation de réservoirs de magma 3 TAIT STEPHEN silicique dans la croûte continentale 4000 Qu'apportent les nouvelles découvertes pétrophysiques à notre compréhension de la 3 Thoraval catherine structure actuelle de la convection mantellique? 3000 Interaction surface/intérieur dans les mondes glacés 3 TOBIE Gabriel du Système solaire. 5500 Hydrocarbures dans la basse atmosphère de Titan : nucléation, condensation et croissance des aérosols 4 Biennier Ludovic 5000

Déstabilisation d?un lit de grains par de l?eau métastable sous conditions de pression martienne. 4 CARPY Sabrina 3000 Composition et dynamique des planètes géantes et 4 Cavalié Thibault de leur système 5500 4 Chaufray Jean-Yves Modélisation 3D de la haute atmosphère de Mars 2000 4 Couturier-Tamburelli IsabellePhotochimie des aérosols de Titan 8500 Organisation d?un atelier francophone intitulé « Traitement d?images multimodales pour 4 Douté Sylvain l?exploration du Système Solaire » 5000 Etude des phénomènes affectant les surfaces glacées de Mars à partir d'observations spectro- 4 Douté Sylvain photométriques et de simulations en laboratoire. 3000 Influence des processus de fonte et sublimation sur la morphologie : de l?histoire de Mars au suivi 4 GARGANI Julien saisonnier 5000 Etude des magnétosphères de la Terre et des 4 Lamy Laurent planètes géantes 6500 4 LAVVAS Panayotis Atmospheric Molecular Growth 6500 Modélisation de l'exosphère d'Europa et Ganymède 4 Leblanc Francois 2500 4 LEBONNOIS Sebastien MEVeTiPPE 4000 4 Lilensten Jean Ionosphère martienne : dications moléculaires 4000 4 Loison Jean-Christophe PHOFEX (PhotoFragments EXcitation) 8500 Observations et modélisation des atmosphères de 4 Maattanen Anni Mars et Vénus 7500 Mesures des paramètres collisionnels de H2O par CO2. Application à l?étude des atmosphères de 4 REGALIA laurence Vénus et Mars. 2000 Exploration du système de bandes inconnues du méthane isotopique dans la fenêtre de 2 microns pour l?interprétation des données des missions 4 TYUTEREV Vladimir spatiales 4000 Etude de l?atmosphère et de Titan à partir des 4 Vinatier Sandrine données Cassini et ALMA 7000 4 Widemann Thomas Observations de la dynamique et la composition de 2000 Comparaison de la chimie de l?océan au 5 BLICHERT-TOFT Janne Protérozoïque et à l?Archéen 9000 Formation de la croûte continentale: différenciation magmatique et devenir des roches mafiques et 5 Jaupart Claude ultramafiques 7000 Environnements, climat et vie à la surface de la Terre Primitive : rôles des facteurs locaux vs. 5 Marin-Carbonne Johannaglobaux 4000 Formation d?une croûte primaire sur la Lune et 5 Michaut Chloé Mars 4500 LE CYCLE DE l?ARSENIC AU PRECAMBRIEN ? 5 PHILIPPOT Pascal ANALOGUES ANDINS 4000 ANNÉE 2018 Nom Prénom Titre du projet thème Financement

ALLARD France Modélisation des atmosphères stellaires et planétaires 1 1000 Modélisation et Simulation des Disques de Débris et AUGEREAU Jean-Charles 1 Exozodiacaux 4500 Mesure de masses des exoplanètes découvertes par BEAULIEU Jean-Philippe 1 microlensing. 4500 Atmosphères des planètes extrasolaires et conditions de BOCCALETTI Anthony 1 formation dans les disques circumstellaires 4500 Recherche et caractérisation de planètes avec le BOISSE Isabelle 1 spectrographe SOPHIE 5000

BONNEFOY Mickael Inversion des Spectres en Emission des exoPlanètes géantes 1 2000 etude du « Bruit » StellaIre pour la Détection d'Exoplanètes CHIAVASSA Andrea 1 et la caractériSation de leurs propriétés 2000 Recherche et caractérisation de planètes autour d'étoiles de DELFOSSE Xavier 1 très faible masse 2000 DELORME Philippe Action Coordonnée Exploitation SPHERE 1 5500

HEBRARD Guillaume Recherche et caractérisation de planètes extrasolaires à l'IAP 1 4000 Etude et modélisation fine d'un nouveau disque de transition LANGLOIS MORETTOMaud 1 détecté sur la tranche par l'instrument SPHERE dans le Upper 2000

LASKAR Jacques Dynamical Interactions in Multi-Planet Systems 1 4000 Participation à un projet international Early Science Release LESTRADE Jean-Francois du JWST dans le but d'étudier les disques de débris en 1 relation avec les exoplanètes 3000 Préparation des observations de disques proto-planétaires Matter Alexis 1 avec l'instrument VLTI/MATISSE 2000 Activité magnétique et recherche de Jupiters chauds autour PETIT Pascal 1 d'étoiles jeunes en rotation rapide 2000 Caractérisation de super-Terres et mini-Neptunes en transit SANTERNE Alexandre 1 avec K2 et HARPS 3000 Caractérisation des atmosphères d'exoplanètes géantes et SELSIS Franck 1 telluriques avec HST, JWST et ARIEL. 3000 Evolution couplée des systèmes étoile-planète par Strugarek Antoine 1 et 3 interactions MHD et marées 3000 Préparation de la mission spatiale JWST : Modélisation VENOT Olivia 1 et 4 Photochimique d'Exoplanètes et Mesures spectroscopiques à 5000 Structure interne, évolution et dynamique atmosphèrique chabrier gilles des planètes solaires et extrasolaires 1 et 2b 2500

DELBO Marco Primitive asteroids and asteroid families 2b 5000 Modélisation hybride N-corps - hydrodynamique de la DUNSEATH Kevin formation de Phobos et Deimos suite à un impact géant 2b 1000 La population des géocroiseurs, traceurs des origines du FORNASIER Sonia système solaire et de l'origine de la vie 2b 6000 Origine des comètes à longue période et stabilité à long Fouchard Marc terme dans la région de l'éventuelle planète 9 2b 2000 Évolution de la porosité des grains de poussière pendant leur GONZALEZ Jean-François croissance : une solution aux problèmes de formation planétaire ? 2b 1500

LAIBE Guillaume Des poussières aux planètes : une approche globale 2b 2500 Dynamique des anneaux de Saturne à la lumière des données LONGARETTI Pierre-Yves Cassini 2b 4000 Modélisation de la formation du système solaire externe pour PETIT Jean-Marc préparer JWST, LSST, EUCLID, ..., et vice-versa 2b 7000

Vaubaillon Jeremie Meteor Automated Light Balloon Experimental Camera 2b 3000 Probing the interior of primordial main belt asteroids with VERNAZZA Pierre VLT/SPHERE 2b 4500 Origine des volatils d'alteration dans les inclusions ALEON Jerome réfractaires des chondrites 2a 8000 CARBOSPIN-II : Radicaux dans des analogues de matière BINET Laurent carbonée extraterrestre 2a 5500

CARTIER Camille Fractionnement métal/silicate dans le Système Solaire 2a 10000 COMET Comet Organic MicromETeorites, étude de DUPRAT Jean l'association entre minéraux et matière organique dans des 2a 7000 poussières cométaires. Les inclusions vitreuses à composition non chondritique dans FAURE François les olivines des chondres de type I: une fenêtre sur la différenciation des protoplanètes? 2a 5000 L'angrite Asuka 12209 : une nouvelle référence pour la GOPEL Christa datation du système solaire précoce 2a 4000 Existe-t-il un lien entre la chimie du milieu interstellaire et GUILLEMIN Jean-Claude celle des comètes ? 2a et 2b 1000 HICKSON Kevin La réactivité des atomes à basse température 2a 5000 Formation et évolution des couronnes à grains fins à LEROUX Hugues l'interface chondre-matrice dans les chondrites carbonées : Application de nouvelles méthodes quantitatives 2a 7500 Interdiffusion hydrogène-deutérium dans les minéraux REYNARD Bruno hydratés terrestres et extraterrestres 5 et 2a 7500 Cosmic Abundance Depletion Origin for intermediate Z SIMIONOVICI Alexandre elements - continuation 2a 5000 Chronologie de formation des chondres et de leurs VILLENEUVE Johan 2a précurseurs 9000 ALBOUSSIERE Thierry Convection compressible avec changement de phase 3 4 500 The South Atlantic Magnetic Anomaly and core-mantle AMIT Hagay 3 4 000 coupling Test de l'origine de l'anomalie DUPAL à l'aide des isotopes AUBAUD Cyril 3 2 000 stables du carbone BOLFAN Nathalie Signature isotopique D/H de la zone de transition 3 7 000 Oxidation state of primitive arc-magma at the crust-mantle Bouilhol Pierre 3 5 000 transition zone BUREAU Helene Le rôle des halogènes dans la zone de transition 3 4 000 Les différents régimes de convection dans un manteau DAVAILLE Anne 3 6 500 planétaire à la fin de la solidification de l'océan de magma. Déformation de surface et dynamique des couches de glace DUMOULIN Caroline 3 et 4 3 000 d'Encelade et d'Europe IACONO MARZIANOGiada Contrôles redox sur le cycle géodynamique du soufre 3 5 000 Non-traditional stable isotopes in the Bulk Silicate Earth and IONOV Dmitri upper mantle from xenolith data, and their fractionation in 5 500 mantle processes 3 Développement d'un modèle d'atténuation de référence de MARGERIN Ludovic 3 2 000 la Lune Calcul Haute performance pour la modélisation et inversion MARTIN Roland d'anomalies gravimétriques aux échelles régionales et 3 3 000 globales : Données sol et satellite (GOCE, DTU et BGI)

Effets de fusion partielle sur la dynamique de la graine MERKEL Sebastien 3 5 500 terrestre PERRIN Mireille Variation séculaire au Kenya 3 7 500 QUESNEL Yoann Géophysique de la structure d'impact Rochechouart 3 et 4 8 000 Développement d'une nouvelle méthode de modélisation du SAMUEL Henri 3 3 500 transport ADVECTif en géodynamique La forme et la formation de réservoirs de magma silicique TAIT Steve 3 5 000 dans la croûte continentale

Hydrocarbures et nitriles dans la basse atmosphère de Titan : BIENNIER Ludovic 4 nucléation, condensation et croissance des aérosols 5500 École thématique GeoPlaNet 2018 : Interactions BOURGEOIS Olivier 4 fluides/roches dans le Système Solaire 2500 Déstabilisation d'un lit de grains par de l'eau soumise à un CARPY Sabrina 4 changement de phase. Etude expérimentale. 4000 Composition et dynamique des planètes géantes et de leurs CAVALIE Thibault 4 systèmes 6500 Chaufray Jean-Yves Modélisation 3D de la haute atmosphère de Mars 4 3500 Titan : Interaction et Spectroscopie Surface-Atmosphère - CORDIER Daniel 4 Généralisation aux Exoplanètes 7500 Evolution photochimique des Aérosols de la Stratosphère de COUTURIER Isabelle 4 Titan 4500 Etude des phénomènes affectant les surfaces glacées de Douté Sylvain Mars à partir d'observations spectro-photométriques et de 4 simulations en laboratoire. 2000 Vers la Mesure dE Rapports de branchement de GANS Bérenger photodissociation VUV pour des Composés d'Intérêt 4 Astrophysique 8000 LAMY Laurent Etude des magnétosphères terrestre et planétaires 4 7500

LEBONNOIS Sebastien Modèles d'Atmosphères de Référence pour la Communauté 4 7000 Observation et modélisation des atmosphères de Mars et LEFEVRE Franck 4 Vénus 7500 Emissions thermiques des sous surfaces planétaires dans le LEYRAT Cedric domaine millimétrique et centimétrique : Etudes de Pluton 4 et des satellites de Saturne. 5000 Détection magnétique des modes propres de Jupiter et de la LOGNONNE Philippe 4 et 3 Terre : Analyse comparée 1000 LOISON Jean-ChristophePhotoFragments EXcitation 4 2000 Etude expérimentale du continuum d'absorption pour un MONDELAIN Didier mélange H2O - CO2 en support à l'analyse et à la 4 modélisation des atmosphères planétaires 2500 Chlorine and Sulfur in martian basaltic magmas: Solubility MORIZET Yann 4 et 3 and speciation. 4500 Cristallisation de sels par sublimation de glace : modélisation RONDEAU Benjamin 4 expérimentale de dépôts planétaires. 2000 Surface d'Europe: Modélisation du cryovolcanisme et micro- SCHMIDT Frederic 4 texture de la surface. 4500 SEJOURNE Antoine Etude des traces de cryosphère ancienne et actuelle 4 5000 Etude de l'atmosphère et de la surface de Titan à partir des VINATIER Sandrine 4 données Cassini et ALMA 7500 Les atmosphères de Vénus et de Mars : Composition, WIDEMANN Thomas 4 dynamique et rapport D/H 2500 BADRO James Experimental Study of Earth's Primordial Magma Ocean 5 et 3 6500 Comparaison de la chimie de l'océan au Protérozoïque et à BLICHERT-TOFTJanne 5 l'Archéen 7500 La croissance crustale Archéenne, une approche multi- Moyen Jean-François 5 isotopes 8000 TOUBOUL Mathieu New Isotopic Tracers of Early Mantle Heterogeneities 3 5 500